COMMISSIONS AND OF THE I A U

INFORMATION BULLETIN ON VARIABLE STARS

Nos

April November

EDITORS L SZABADOS K OLAH

TECHNICAL EDITOR A HOLL

TYPESETTING MB POCS

ADMINISTRATION Zs KOVARI

EDITORIAL BOARD E Budding HW Duerb eck EF Guinan

P Harmanec chair D Kurtz KC Leung C Maceroni

NN Samus advisor C Sterken advisor

H BUDAPEST XI I Box HUNGARY

URL httpwwwkonkolyhuIBVSIBVShtml HU ISSN

2 IBVS 4701 { 4800

COPYRIGHT NOTICE

IBVS is published on b ehalf of the th and nd Commissions of the IAU by the

Konkoly Observatory Budap est Hungary

Individual issues could b e downloaded for scientic and educational purp oses free of

charge Bibliographic information of the recent issues could b e entered to indexing sys

tems No IBVS issues may b e stored in a public retrieval system in any form or by any

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Prior written p ermission of the publishers is required for entering IBVS issues to

an electronic indexing or bibliographic system to o

IBVS 4701 { 4800 3

CONTENTS

WOLFGANG MOSCHNER ENRIQUE GARCIAMELENDO

GSC A New Variable in the Field of V Cassiop eiae ::::::::::

JM GOMEZFORRELLAD E GARCIAMELENDO J GUARROFLO

J NOMENTORRES J VIDALSAINZ

Observations of Selected HIPPARCOS Variables :::::::::::::::::::::::::::

JM GOMEZFORRELLAD

HD a New Low Amplitude Variable Star ::::::::::::::::::::::::::

ME VAN DEN ANCKER AW VOLP MR PEREZ D DE WINTER

NearIR Photometry and Optical Sp ectroscopy of the Herbig Ae Star AB Au

rigae ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::::::::

KEVIN KRISCIUNAS AND BRIAN M PATTEN

Dor Candidates in the Op en Cluster M ::::::::::::::::::::::::::::::::

R HAEFNER V Aql An Eclipsing Classical Nova :::::::::::::::::::::

T KIPPER The Dust Shell Around Sakurais Ob ject ::::::::::::::::::::::

JENNWOOD CHEN T MICHAEL CORWIN

BV Photometry of SX Phe Blue Stragglers in the Globular Cluster NGC



GLENN GOMBERT BD a New UU Herculis Variable :::::::::

PETR MOLIK MIROSLAV BROZ MAREK WOLF

CCD Photometry of V Cassiop eiae :::::::::::::::::::::::::::::::::::::

FRANZ AGERER JOACHIM HUBSCHER

Photo electric Minima of Selected Eclipsing Binaries ::::::::::::::::::::::::

FRANZ AGERER MICHAEL DAHM JOACHIM HUBSCHER

Photo electric Minima of Selected Eclipsing Binaries and Maxima of Pulsating

Stars ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::::::::::::::

H ROVITHISLIVANIOU A KRANIDIOTIS E FRAGOULOPOULOU

N SERGIS P ROVITHIS On the Orbital Period Changes of AK Herculis :

RM ROBB DD BALAM AND R GREIMEL Discovery of the Optical

RXS J :::::::::::: Variability of the Star GSC

T J REYNOLDS J R THORSTENSEN AND N D SHERMAN

Variable Stars Near V Aql Aql X :::::::::::::::::::::::::::::::

CHULHEE KIM A Susp ected Variable Ob ject in the Field of C :::::::

R DIETHELM GSC a Newly Discovered Variable Star :::::::::

SV ANTIPIN NA GORYNYA ME SACHKOV NN SAMUS

LN BERDNIKOV AS RASTORGOUEV EV GLUSHKOVA



The Radial Velocity of Doublemo de Cepheid BD ::::::::::::::::

BRIAN A SKIFF

Co ordinates and Identications for Sonneb erg Variables I :::::::::::::::::

BRIAN A SKIFF

Co ordinates and Identications for Sonneb erg variables II ::::::::::::::::

BRIAN A SKIFF

Co ordinates and Identications for Sonneb erg variables III ::::::::::::::

BRIAN A SKIFF FASTT versus IRAS :::::::::::::::::::::::::::::::::::

BRIAN A SKIFF

Co ordinates and Identications for Kuro chkins variables near M :::::::::

4 IBVS 4701 { 4800

L N BERDNIKOV V V IGNATOVA D G TURNER Photo electric BVI

c

Observations and New Elements for the Cepheid V Centauri ::::::::::::

L N BERDNIKOV D G TURNER

Photo electric VI Observations and New Classication for RV Normae ::::::

c

J VANDENBROERE NSV a Lyrae Type Eclipsing Binary :::::::

T RUSSEVA V V and Four New Variable Stars in the Field of M ::::

PRISCILLA J BENSON AND DEMERESE M SALTER

GSC A Susp ected New Variable :::::::::::::::::::::::::::::::

SAUL J ADELMAN

StromgrenPhotometry of the Be Star  CrB :::::::::::::::::::

YURIJ N KRUGLY GSC is a New Variable Star :::::::::::::::

HILMAR W DUERBECK Hipparcos Parallaxes of Cataclysmic Binaries and

the Quest for Their Absolute Magnitudes ::::::::::::::::::::::::::::::::::

P MERCHANBENITEZ M JURADOVARGAS F SANCHEZBAJO

Photometric Observations of NSV :::::::::::::::::::::::::::::::::::

JD FERNIE A Photometric Up date on  Coronae Borealis :::::::::::::::

LENNART DAHLMARK New Variable Stars in Andromeda and Cassiop eia

PK ABOLMASOV SYU SHUGAROV

Discovery of a New Mira Variable :::::::::::::::::::::::::::::::::::::::::

SEI ICHIRO KIYOTA Photometry of the outburst of U Scorpii :::::::

CLAUD H SANDBERG LACY KYLE MARCRUM CAFER IBANOGLU

Times of Minima of Eclipsing Binaries :::::::::::::::::::::::::::::::::::::

F J CLARKE T A LISTER

CCD Lightcurves and Minima Times of the Eclipsing Binary RZ Cas :::::::

Z KVIZ y M ZEJDA L KOHOUTEK J GRYGAR

Times of Minima of Some Southern Eclipsing Binaries :::::::::::::::::::::

IOAN TODORAN RODICA ROMAN RZ Cephei Period Variation ::::

LIU YY Photometry of the  Scuti Star HR ::::::::::::::::::::::::

B HASSFORTHER U BASTIAN

IRAS A New Mira Variable :::::::::::::::::::::::::::::::::::

AS MIROSHNICHENKO KS KURATOV TA SHEIKINA



DB MUKANOV LS i i a Newly Recognized Classical Be star :::::

V SIMON S SHUGAROV

Rise from the Low State of the Binary V Sagittae ::::::::::::::::::::::::::

T KATO CCD Photometry of BF Eridani a Lowamplitude Dwarf Nova

SEI ICHI YOSHIDA KENICHI KADOTA

New Variable Stars Discovered in the MISAO Pro ject I MisVMisV

E PORETTI The light curves of SX Phe stars in NGC ::::::::::::::

M ZBORIL J BUDAJ

Dierential UBV photometry of two CP stars Her and Her ::::::::::

J R THORSTENSEN

The Sp ectrum Period and Prop er Motion of V Scorpii :::::::::::::::::

ROGER DIETHELM MAREK WOLF

CCD Photometry of the Eclipsing Binary V Cygni ::::::::::::::::::::

Erratum ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::::

T PRIBULLA D CHOCHOL S PARIMUCHA

Photo electric Minima of Some Eclipsing Systems :::::::::::::::::::::::::::

JM DEPASQUALE JJ BOCHANSKI EF GUINAN Recent Light Curves

and Period Study of the Contact Binary W Ursae Ma joris ::::::::::::::::::

IBVS 4701 { 4800 5

RONALD G SAMEC NW GOTHARD BC PARKER TW SAVAGE

SD ANDERSON DANNY R FAULKNER

UBV Observations of the Mass Exchanging SolarType Binary BE Cephei ::

RAYMOND H BLOOMER JR ISSA R NGWELE

Comments on the Light Curve of V Her ::::::::::::::::::::::::::::::::

CLAUD H SANDBERG LACY AND JEFFREY A SABBY

Absolute Prop erties of ZZ Ursae Ma joris :::::::::::::::::::::::::::::::::::

P MERCHANBENITEZ M JURADOVARGAS F SANCHEZBAJO

NSV an RR Lyrae Type Star in Libra ::::::::::::::::::::::::::::::

T KATO P SCHMEER

CCD Photometry of the February Outburst of CI Gem :::::::::::::::

PATRICK SCHMEER AND HILMAR W DUERBECK

The February Outburst of the Dwarf Nova CI Gem :::::::::::::::::::

HILMAR W DUERBECK PATRICK SCHMEER JOHAN H KNAPEN

DON POLLACCO The February Sup eroutburst of the SU UMatype

Dwarf Nova CG CMa ::::::::::::::::::::::::::::::::::::::::::::::::::: ::

T KATO K MATSUMOTO R STUBBINGS

CCD Photometry of the Outburst of CG CMa ::::::::::::::::::::::::

T KATO Precise Co ordinates of Variable Stars ::::::::::::::::::::::::

T KATO Precise Co ordinates of Variable Stars ::::::::::::::::::::::::

T KATO K MATSUMOTO

CCD Photometry of the February Sup eroutburst of CY UMa :::::::::

T KATO Precise Co ordinates of Variable Stars ::::::::::::::::::::::::

T KATO K MATSUMOTO CCD Observation of the Octob er Sup er

outburst of PU Per Conrmation as an SU UMatype Dwarf Nova :::::::::

T KATO D NOGAMI H BABA Cyclic Variability of V Aql ::::::::

T KATO K MATSUMOTO

CCD Photometry of the December Outburst of AQ Eri :::::::::::::::

T KATO CCD Photometry of the March Outburst of BZ UMa Detec

tion of QuasiPeriodic Oscillations :::::::::::::::::::::::::::::::::::::::::

T KATO Orbital Mo dulation During the Standstill of VW Vul ::::::::::::

SEI ICHI YOSHIDA KENICHI KADOTA TAICHI KATO New Variable

Stars Discovered in the MISAO Pro ject I I MisVMisV :::::::::::

SEI ICHI YOSHIDA KENICHI KADOTA TAICHI KATO New Variable

Stars Discovered in the MISAO Pro ject I I I MisVMisV :::::::::::

SV ANTIPIN A New Classical Cepheid in Sagitta ::::::::::::::::::::::::

NN SAMUS L HAYTHE S HORNSTEIN LJ JISONNA JR E LU

Lost Variables on Nantucket Plates ::::::::::::::::::::::::::::::::::::::::

WILLIAM LILLER ALBERT JONES

Light Curves for Nova Mus and Nova Oph :::::::::::::::::::::::

T ARENTOFT AND C STERKEN A New Dor Candidate in Crux :::::

T KATO K MATSUMOTO

CCD Observation of the November Outburst of V Peg An SU UMa

type Dwarf Nova With a Long Orbital Period ::::::::::::::::::::::::::::

T KATO M UEMURA R STUBBINGS T WATANABE B MONARD

Preoutburst Activity of V Sgr SAX J Possible Existence

of Day Period ::::::::::::::::::::::::::::::::::::::::::::::::::: ::::::

FRANZ AGERER New Elements and Light Curve of CR Tauri ::::::::::::

6 IBVS 4701 { 4800

N BENNERT I KONIG E MANTHEY H BLEUL K FIEGER M HESS

A HOVEST W HOVEST T JURGES J KLEIMANN

C KRIEGESKORTE E KRUSCH D MUNSTERMANN D REYMANN

K ROSLER M NIELBOCK M POHLEN L SCHMIDTOBREICK

C TAPPERT R VANSCHEIDT

Dierential Photometry of Susp ected Cataclysmic Variables ::::::::::::::::

SEI ICHI YOSHIDA KENICHI KADOTA TAICHI KATO New Variable

Stars Discovered in the MISAO Pro ject IV MisVMisV :::::::::::

NA SOKOLOV Variations in the Eective Temperature and the Balmer

Jump of the Ap Star Tauri :::::::::::::::::::::::::::::::::::::::::::::

CLAUD H LACY MAMNUN ZAKIROV GC ARZUMANYANTS

NR BAIRAMOV AS HOJAEV New Analyses of V Cygni Light Curves

ENRIQUE GARCIAMELENDO FLORENTINO SANCHEZBAJO

NSV is a Short Period Variable in Ophiuchus ::::::::::::::::::::::::

F FAGHIHI N RIAZI A DARIUSH UBV Photo electric Times of Minima

of the Eclipsing Variable TV Cassiop eiae ::::::::::::::::::::::::::::::::::

D MORO U MUNARI T TOMOV A HENDEN

The Precursor of Nova Aquilae V Aql :::::::::::::::::::::::::

T KATO M UEMURA CCD Observation of the Fading of LQ Peg :

T KATO M UEMURA

CCD Observation of the September Outburst of TY Vul ::::::::::::::

T KATO Precise Co ordinates of Variable Stars ::::::::::::::::::::::::

T KATO Precise Co ordinates of Variable Stars ::::::::::::::::::::::::

T KATO Precise Co ordinates of Variable Stars ::::::::::::::::::::::::

T KATO Precise Co ordinates of Variable Stars ::::::::::::::::::::::::

SEI ICHI YOSHIDA KENICHI KADOTA TAICHI KATO

Possible Identication of MisV and NSV ::::::::::::::::::::::::

SEI ICHI YOSHIDA KENICHI KADOTA TAICHI KATO New Variable

Stars Discovered in the MISAO Pro ject V MisVMisV :::::::::::

T KATO S KIYOTA R NOVAK K MATSUMOTO

CCD Photometry of the February Sup eroutburst of CT Hya ::::::::::

T KATO M UEMURA

Identication and CCD Photometry of Luytens GM Sgr :::::::::::::::::::

ERIC G HINTZ MAUREEN L HINTZ MICHAEL D JONER AND

LISA A JONER Reduced Amplitude of V Ophiuchi :::::::::::::::::::

C LLOYD K BERNHARD P FRANK W MOSCHNER Discovery of the

Variability of GSC GSC and GSC :::::::::::::

FRANZ AGERER THOMAS BERTHOLD PETER KROLL

The Variable Period of V Cassiop eiae ::::::::::::::::::::::::::::::::::

T KATO Precise Co ordinates of Variable Stars ::::::::::::::::::::::::

RM ROBB J WAGG A BERNDSEN AND L DESROCHES Photometry

RXS J ::::::: of the Eclipsing Binary Star GSC

IBVS 4701 { 4800 7

AUTHOR INDEX

Ab olmasov PK Grygar J

Adelman SJ GuarroFlo J

Agerer F Guinan EF

Anderson SD Haefner R

Antipin SV Hassforther B

Arentoft T Haythe L

Arzumanyants GC Henden A

Baba H Hess M

Bairamov NR Hintz EG

Balam DD Hintz ML

Bastian U Ho jaev AS

Bennert N Hornstein S

Benson PJ Hovest A

Berdnikov LN Hovest W

Berndsen A H ubscher J

Bernhard K Ibanoglu C

Berthold T Ignatova VV

Bleul H Jisonna LJ Jr

Blo omer RH Jr Joner LA

Bo chanski JJ Joner MD

BrozM Jones A

Buda j J JuradoVargas M

Chen J J urges T

Cho chol D Kadota K

Clarke FJ

Corwin TM Kato T

Dahlmark L

Dahm M

Dariush A

de Winter D

DePasquale JM

Desro ches L

Diethelm R Kim Ch

Duerb eck HW Kipp er T

Faghihi F Kiyota S

Faulkner DR Kleimann J

Fernie JD Knap en JH

Fieger K Kohoutek L

Fragoulopoulou E KonigI

Frank P Kranidiotis A

GarciaMelendo E Kriegeskorte C

Glushkova EV Krisciunas K

Gombert G Kroll P

GomezForrellad JM Krugly YuN

Gorynya NA Krusch E

Gothard NW Kuratov KS

Greimel R KvzZ

8 IBVS 4701 { 4800

Lacy CH Schmeer P

Liller W Schmidtobreick L

Sergis N

Lister TA

Sheikina TA

Liu YY

Sherman ND

Lloyd C

Shugarov S

Lu E

Shugarov SYu

Manthey E

Ski BA

Marcrum K

Sokolov NA

Matsumoto K

Sterken C

Stubbings R

MerchanBentezP

Simon V

Miroshnichenko AS

Tappert C

MolkP

Thorstensen JR

Monard B

Todoran I

Moro D

Tomov T

Moschner W

Turner DG

Mukanov DB

Uemura M

Munari U

van den Ancker ME

M unstermannD

Vandenbroere J

Ngwele IR

Vanscheidt R

Nielb o ck M

VidalSainz J

Nogami D

Volp AW

NomenTorres J

Wagg J

NovakR

Watanabe T

Parimucha S

Wolf M

Parker BC

Yoshida S

Patten BM

PerezMR

Zakirov M

Pohlen M

Zb oril M

Pollaco D

Zejda M

Poretti E

Pribulla T

Rastorgouev AS

Reymann D

Reynolds TJ

Riazi N

Robb RM

Roman R

Rovithis P

RovithisLivaniou H

RoslerK

Russeva T

Sabby JA

Sachkov ME

Salter DM

Samec RG

Samus NN

Savage TW

SanchezBa jo F

IBVS 4701 { 4800 9

INDEX OF VARIABLES

The extensive lists of variable stars published in the IBVSissues Nos

and are not

rep eated here

Star IBVS No Star IBVS No

RT And U Col

RX

T CrB

HQ

Delta

AE Aqr Theta

V Aql SS Cyg

V V

V V

V V

V

HR Del

T Aur

HI Dra

SS

AQ Eri

AB

BF

HM

U Gem

i Bo o

CI

SV Cam

AK Her

WW

DQ

WY Cnc

V

XX CMa V

CG

TU Car

QU CT Hya

RZ Cas RW Lac

TV

ET Leo

V

V Lep

V

RS

V

RU

V

UX Men

V

BS Mon

V

BT

DL Cen

HW

V

W Mus

RZ Cep

RV Nor

VW

WW

V Oph

BE

V Ori

EG

V

10 IBVS 4701 { 4800

Star IBVS No Star IBVS No

FBS LQ Peg

FBS

PU

V

GSC

V

GSC

GSC

FO Per

GSC

PU

GSC

Zeta Phe

GSC

RR Pic

GSC

BO Pup

GSC

ES

GSC

GSC

V Sge

HD

BC Sgr

BQ

HIP

BY

HR

CU

IRAS

GM

IRAS

V

LD LD

V



LS II

V

MisVMisV

U Sco

MisVMisV

V

MisV

UW Sct

MisVMisV

ZZ

MisVMisV

AE

MisVMisV

BC

Nova Mus

RW Sex

Nova Oph

CR Tau

NSV

GS

NSV

W UMa

NSV

XY

NSV

ZZ

NSV

AW

NSV

BZ

NSV

CY

Variables in Clusters

AD Vel

in M

CW

in M

IX

in NGC

TY Vul

in NGC

VW

BP

New Variables

ER

in the eld of C





BD

BD



BD GSC

IBVS 4701 { 4800 11

Star IBVS No

GSC

GSC

GSC

GSC

GSC

GSC

GSC

GSC

HD

HIP

IRAS

IRAS

LD LD

in M

in the eld of M

MisVMisV

MisVMisV

MisVMisV

MisVMisV

MisVMisV

h m s

R:A:

 0 00

Decl:

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

GSC A NEW VARIABLE

IN THE FIELD OF V CASSIOPEIAE

1 2

WOLFGANG MOSCHNER ENRIQUE GARCIAMELENDO

1

Bundesdeutsche Arb eitsgemeinschaft f ur Veranderliche Sterne eV BAV Munsterdamm D

Berlin Germany email wolfgangmoschnertonlinede

2

Esteve Duran Observatory El MontanyaSeva Seva Barcelona Spain

email duranobsastrogeacescaes

Name of the ob ject

GSC

Equatorial co ordinates Equinox

h m s  0 00

RA DEC

Observatory and telescop e

Private Observatory in Lennestadt m RitcheyChretien telescop e Esteve Du

ran Observatory m Cassegrain telescop e

Detector CCD

Filters V

Comparison stars GSC

Check stars GSC GSC

Transformed to a standard system No

Availability of the data

Through IBVS Website as ttxt

Type of variability DSCT

IBVS

Remarks

The variability of GSC was found while b eing used as comparison star

for V Cas CCD observations show that this ob ject has light variations with an

amplitude in the V band close to magnitude and a p erio d of 

days The shap e of the light curve indicates that this variable is not an ellipsoidal

nor eclipsing binary system Although the p erio d has remained stable for almost a

year from Octob er to Octob er the light curve shows instabilities

from cycle to cycle similar to those of a Delta Sct star To derive more informa

its average B V color index was estimated using the tion ab out GSC

TYCHO star GSC Photometric data showed that B V 

This value is redder than the typical one for a Delta Sct variable but GSC

is near the Galactic plane and it might b e aected by interstellar extinction Fig

folded according to the given p erio d ure shows the light curve of GSC

To construct Figure and due to light curve instabilities the zero ep o ch was arbi

trarily xed

Acknowledgements

This research made use of the SIMBAD data base op erated by the CDS at Stras

b ourg France Figure

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

OBSERVATIONS OF SELECTED HIPPARCOS VARIABLES

1 2 1

JM GOMEZFORRELLAD E GARCIAMELENDO J GUARROFLO

1 1

J NOMENTORRES J VIDALSAINZ

1

Grup dEstudis Astronomics Apartado Barcelona Spain email jmgomezastrogeacescaes

2

Esteve Duran Observatory Foundation El MontanyaSeva Seva Barcelona Spain

email duranobsastrogeacescaes

New photometric observations of nine HIPPARCOS variables p erformed b etween

and are presented Most of these stars were selected on the basis of a new analysis

of the satellite data which suggested that the actual type of variability could b e dierent

from the originally listed in the HIPPARCOS and TYCHO catalogues ESA In

the th Sp ecial Namelist Kazarovets et al some of these observed stars were

correctly reclassied but the new data showed that still some of them are improp erly

classied In all cases observations allowed to improve the existing satellite light curve

and ephemeris Table lists the observational log for these ob jects whereas Table

summarizes the obtained results

Table

HIP Observational interval Comparison Check stars Remarks

Nov Jan SAO SAO

Oct Feb SAO HD

Jan Jan PPM PPM

Dec Mar SAO

Mar Jul SAO GSC

Aug Oct GSC

Jun Oct SAO

Aug Sep SAO

Sep Oct SAO SAO

SAO

Remarks to Table

Piera Observatory cm telescop e Esteve Duran Observatory cm telescop e

Mollet del Valles Observatory cm telescop e LEstelot Observatory cm telescop e

Monegrillo Observatory cm telesop e Esteve Duran Observatory cm telescop e

Mollet del Valles Observatory cm telescop e

V Cas Catalogued as an EW in the th Sp ecial NameList This ob ject was also

included in a list of low amplitude EW system candidates by Duerb eck New pho

tometric observations conrm the binary nature of this star an EW undergoing marginal

IBVS

Table



HIP GCVSName V mag range Sp ectral type Variable type

V Cas F EW or ELL

V Cas B EA

V Ori F EW or ELL

ET Leo G EW or ELL

A EA

HI Dra F EB or ELL

V Aql A EA

PU Peg F EB

V Peg AI I I EW



When two magnitude ranges are given the rst one corresp onds to minimum I and

the second one to minimum I I

eclipses or an ellipsoidal variable Figure

d

Min I HJD  E

 

V Cas Classied as an EB eclipsing binary system the new photometric data

indicate that this ob ject is actually an Algoltype variable Figure and conrm the

original HIPPARCOS ephemeris The following primary minimum timing was derived

Min I HJD ep o ch



V Ori This star was classied as EW with a p erio d of days and brightness

m m

variation from to in the V band ESA In the th Sp ecial Name

List the star was catalogued as an EW New data show that this ob ject is an EW or ELL

m

variable Figure A OConnell eect Max I Max I I Max I is the maximum

following the primary minimum also present in the folded HIPPARCOS light curve was

detected

d

Min I HJD  E

 

ET Leo Initially listed as an unknown variability type with a p erio d of

m m

days and a brightness variation from to in the V band ESA In the

th Sp ecial NameList the star was catalogued as an EW The ob ject was also included

in a list of EW binary stars candidates of low amplitude by Duerb eck Observations

show that it is a W UMa star undergoing marginal eclipses or an ELL Figure

d

Min I HJD  E

 

HIP This ob ject was catalogued as an unsolved variable with a brightness

m m

variation from to ESA Photometric observations showed that

it is an Algoltype ob ject Figure The p osition of the secondary minimum at phase

also suggests that the orbit might not b e circular

d

Min I HJD  E

 

IBVS

Figure Figure

Figure Figure

HI Dra Star listed in the HIPPARCOS catalogue and later classied in the th Sp ecial

NameList as an RRc variable An analysis of the satellite data indicated that this

ob ject was probably an ellipsoidal or Beta Lyrae variable New photometric observations

conrmed that light variations are due to binarity Figure In addition the folded light

m

curve shows an OConnell eect of also present in the folded HIPPARCOS light

curve

d

Min I HJD  E

 

V Aql In the th Sp ecial Namelist of Variable Stars this ob ject is listed as E

An analysis of the photometric satellite data allowed to determine that it is an Algoltype

eclipsing binary star New photometric observations conrmed this p oint Figure

d

 E Min I HJD

 

PU Peg Light curve is depicted in Figure

d

Min I HJD  E

 

V Peg Star catalogued as an RRc variable in the HIPPARCOS catalogue and

in the th Sp ecial Namelist An analysis of the satellite data and new photometric

observations showed that this star is not an RRc Lyrae star but an EW eclipsing binary

system Figure Minimum I and II cannot b e unambiguously distinguished from the

observations In the given ephemeris the b est observed minimum was taken as the primary

one

d

Min I HJD  E

 

IBVS

Figure Figure

Figure Figure

Figure

References

Duerb eck H W IBVS No

ESA The Hipparcos and Tycho Catalogues ESA SP

Kazarovets AV Samus NN Durlevich OV Frolov SV Antipin SV Kireeva

NN Pastukhova EE IBVS No

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

HD A NEW LOW AMPLITUDE VARIABLE STAR

JM GOMEZFORRELLAD

Grup dEstudis Astronomics Apartat Barcelona Spain email jmgomezastrogeacescaes

Name of the ob ject

 

HD SAO PPM BD AGK

GSC

Equatorial co ordinates Equinox

h m s  0 00

RA DEC

Observatory and telescop e

Mollet del Valles Observatory m Newtonian telescop e

Detector CCD

Filters V

Comparison stars HD SAO PPM

 

BD AGK GSC

Check stars No suitable check star was available within the CCD

frames

Transformed to a standard system No

Availability of the data

Up on request

Type of variability Unknown

IBVS

Remarks

HD is a B or B star with a V magnitude of It was found variable

while used as comparison star for V Aql Photometric observations show a

brightness variation of magnitudes with a p erio d of days The light

curve is slightly asymmetric and it is not p ossible to establish the type of variability

Data cannot b e satisfactorily overlapped after b eing folded with a double p erio d

so it is probably not an ellipsoidal variable Another p ossibility is a Per SPB

pulsating ob ject Nevertheless the prewhitened light curve after removing the

main frequency comp onent do es not show additional p erio dicities According to

Waelkens Per stars sometimes must b e observed for more than one season

to detect multiperio dicity It may also b e a Bp star but there is insucient sp ectral

information to supp ort this hypothesis The following ephemeris was computed

d

Max HJD  E

 

Acknowledgements

For this research the SIMBAD database op erated by CDS Strasb ourg France has

b een utilized

Figure

Reference

Waelkens C in New Perspectives on Stel lar Pulsation and Pulsating Variable Stars

Nemec JM and Matthews JM editors Cambridge University Press p

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

NEARIR PHOTOMETRY AND OPTICAL SPECTROSCOPY

OF THE HERBIG Ae STAR AB AURIGAE

1 1 2 3

ME VAN DEN ANCKER AW VOLP MR PEREZ D DE WINTER

1

Astronomical Institute University of Amsterdam Kruislaan SJ Amsterdam The Netherlands

Email marioastrouvanl

2

SMA Corp Largo Drive West Suite Largo MD USA

3

Instituto de Astrofsicade Canarias C Via Lacteasn La Laguna Tenerife Spain

AB Aur HD AVesh is often considered prototypical of the class of Herbig

Ae stars optically visible premain sequence stars of intermediate mass surrounded by

circumstellar disks of dust and gas Its photometric and sp ectral prop erties are well

studied over a wide wavelength range eg Bohm Catala Grady et al van

den Ancker et al Catala et al Although photographic measurements in the

b eginning of this century Gap oschkin and references therein showed the star to b e

strongly variable it has remained nearly constant Herbst et al van den Ancker et al

until a fading of  magnitude in brightness from Nov to Dec rep orted

by amateur observers Kawabata et al and references therein Such an event had

not b een observed since the start of photo electric measurements of AB Aur more than

years ago Although puzzling this rep ort did not trigger immediate resp onse from the

astronomical community since such irregular photometric b ehaviour is known to o ccur in

other Herbig Ae stars and is attributed in these systems to variable extinction towards the

central star by dust clouds moving in and out of our line of sight However a recent IAU

circular Ashok et al rep orts that in January the nearinfrared brightness

of AB Aur due to thermal emission from dust in the circumstellar disk has decreased

by more than a magnitude and the Pa and Br lines known to b e prominent from

literature Harvey Evans et al Nisini et al Ro dgers Woo den

are no longer present in emission These observations suggest that the optical event at

the end of might b e related to an EXOR event after the prototype EX Lup Herbig

Herbst et al in which a considerable part of the inner circumstellar disk

seen nearly edgeon was accreted as opp osed to an UXOR event after UX Ori Bib o

The Grinin et al in which matter moves in and out of our line of sight but

in which the total amount of dust do es not change

To further investigate the changes in the AB Aur system we have obtained new near

IR photometry of AB Aur using the m Carlos Sanchez Telescope CST at the Iza na

observatory on Tenerife on April JD The data were taken through

00

a diaphragm and reduced in a standard fashion The resulting magnitudes J

 H  K  are ab out a magnitude brighter than

the ones rep orted by Ashok et al and are only marginally fainter than older

IBVS

Figure Merged optical sp ectra of AB Aur taken on April with ISIS at WHT

literature values Strom et al Cohen Schwartz Lorenzetti et al

Berrilli et al On April optical sp ectra of AB Aur in the

1 1

A at JD A pixel and A at JD A pixel

wavelength ranges were obtained in service mo de with the ISIS sp ectrograph on the m

William Herschel Telescope WHT at La Palma The sp ectra were reduced with the usual

steps of bias subtraction atelding background subtraction and sp ectral extraction and

wavelength and ux calibration Since the night in which the sp ectra were taken was not

of photometric quality the absolute uxes of the sp ectra were scaled to photometric

literature values and they were merged into one single sp ectrum Fig A plot in which

the continuum has b een normalized to and in which some of the features are identied

is shown in Fig

In our new AB Aur sp ectral data emission comp onents are clearly present in H i H

H and the Paschen lines up to P He i Na i O i and the red Ca i i triplet Except for

the chromospheric He i emission at and A which app ears somewhat stronger

the relative strength of all sp ectral features are within errors equal to those given in the

sp ectral atlas of AB Aur by Bohm Catala Strong variability of the He i emission

strength was already noted by those as well as by other authors Catala et al

Our He i line strengths are within the range of values found in literature

The new nearIR photometry and optical sp ectroscopy of AB Aur presented here shows

that if the rep orted infrared variability is real the system has returned to its normal

inactive state within days of the measurements taken by Ashok et al If

the previous active phase was due to an EXORlike enhanced accretion episo de the

mechanisms resp onsible for keeping the circumstellar disk stable must therefore have replenished the inner disk material with material from the outer disk within this p erio d

IBVS

Figure Normalized optical sp ectra of AB Aur with the most prominent features identied

IBVS

Acknowledgements MvdA acknowledges nancial supp ort through NWONFRA grant

The WHT is op erated on the island of La Palma by the Isaac Newton Group

in the Spanish Observatorio del Ro que de los Muchachos of the Instituto de Astrofsica

de Canarias

References

Ashok NM Chandrasekhar T Bhatt HC Mano j P IAU Circ No

Berrilli F Lorenzetti D Saraceno P Strafella F MNRAS

Bib o EA ThePS AA

BohmT Catala C AAS

Catala C BohmT Donati JF Semel M AA

Catala C BohmT Donati JF Simon T Jiang S Zhao F AA

Catala C Donati JF BohmT Landstreet J et al AA in press

Cohen M Schwartz RD MNRAS

Evans NJ Levreault RM Beckwith S Skrutskie M ApJ

Gap oschkin S Harvard Ann

Grady CA PerezMR Bjorkman KS Massa D ApJ

Grinin VP Rostop china AN Shakhovskoi DN Pisma Astron Zh

Harvey PM PASP

Herbig GH ApJ

Herbst W Herbst DK Grossman EJ AJ

Kawabata T Kogure T Fuji M Ayani K Suzuki M IAU Inf Bul l Var

Stars No

Lorenzetti D Saraceno P Strafella F ApJ

Nisini B Millilo A Saraceno P Vitali F AA

Ro dgers B Woo den DH p oster presented at Protostars Planets IV Santa

Barbara Cal

Strom SE Strom KE Yost J Carrasco L Grasdalen G ApJ

van den Ancker ME de Winter D Tjin A Djie HRE AA

van den Ancker ME Bouwman J Wesselius PR Waters LBFM Dougherty SM

van Disho eck EF AA in press

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

Dor CANDIDATES IN THE OPEN CLUSTER M

1 2

KEVIN KRISCIUNAS AND BRIAN M PATTEN

1

Department of Astronomy University of Washington Box Seattle WA USA

email kevinastrowashingtonedu

2

HarvardSmithsonian Center for Astrophysics Garden Street Cambridge MA USA

email bpattencfaharvardedu

The Dor stars are early Ftype stars lo cated on or near the main sequence in the HR

diagram either at or just redward of the co ol red edge of the Scuti instability strip

Dor variables as a class are nonradial gravitymode pulsators Krisciunas In

Krisciunas Crowe suggested that six early Ftype stars in the op en cluster M

NGC showed evidence for photometric variability over the course of a given night

or from night to night From September to Octob er UT we obtained CCD

timeseries photometry for four of these six stars in two overlapping  arcmin

elds which we call A and B in the central region of M The data were taken with the

USNO m reector lo cated near Flagsta Arizona using a  CCD and broad

0

band lters with eective wavelengths of A and A These lters designated g

0

and r are identical to those b eing used for the Sloan Digital Sky Survey Fukugita et al

In this pap er we shall refer to the M stars by their UVa numbers Ianna

Schlemmer

The primary goal of our timeseries survey was to characterize the relative levels of

variability amongst M member stars not to measure absolute photometry To that

end we elected to use an ensemble averaging technique where the mean magnitude of a

set of demonstrably constant stars at each of the sky p ositions was used as the reference

magnitude for dierential photometry In order to select a set of constant stars for each

p osition we used an iterative approach where we started by using all of our program

stars in each p osition for the ensemble average stars in p osition A and and stars

in p osition B and then rejecting those stars with the largest variations with resp ect to

the reference magnitude In the end we selected stars in p osition A and stars in

p osition B for the ensemble average determinations These stars show variations of 

mmag with resp ect to the ensemble average in their p ositions and thus set the limit for

the amplitude of variations we are able to detect in the remaining program stars

We note that two previously susp ected variable stars UVa and UVa Krisciunas

Crowe are now b elieved to b e constant In fact b oth of these stars are used

as a part of the reference ensemble for p osition A in M Welch Stetson have

devised a simple index for determining whether a star is variable If the variability is

due to a temp erature eect eg pulsations or rotational mo dulation due to star sp ots

the variations observed in one broadband lter should b e correlated with the variations

in another lter For noiseless photometry of an ideal temp eraturevariable star using

IBVS

0 0

two wavelengthadjacent lters such as g and r the WelchStetson variability index

would b e If twolter photometry gives a WelchStetson index of for a given

star then it is not temp eraturevariable For our two ensemble average stars and former

susp ected variables UVa and we derive WelchStetson variability indices of

and This result when combined with a visual insp ection of the light curves

and a lack of any strong p eaks in their Fourier p ower sp ectra show that these stars are

demonstrably constant

Our timeseries campaign revealed a number of new variable stars The Dor candi

dates are discussed here while the co oler variables likely sp otted stars will b e the sub ject

of a separate pap er Patten Krisciunas The two Dor candidates are UVa

lo cated in p osition A of the survey and UVa lo cated in p osition B of the survey

UVa has a WelchStetson variability index of and shows evidence for two

p erio ds P and P days with false alarm probabilities of and

1 2

0

resp ectively The g data are characterized by sinusoids with amplitudes ie

half of p eaktop eak of  and  mmag resp ectively We have combined

0

the Vband data of with the g data of normalizing each to the mean values

of the two observing runs In Figure we show the combined data for the two observing

seasons folded by P but without prewhitening by P For those Dor stars which

1 2

have b een wellcharacterized it has b een found that while the photometric amplitudes of

individual stars may b e variable the p erio ds are often quite stable Figure shows that

this holds true for UVa That the combined photometry folds well strongly suggests

that we have measured the true principal p erio d and not settled on an alias of this p erio d

UVa was our b est Dor candidate in M from scanty observations made in

September The twolter photometry of yields a WelchStetson variability

index of not a particularly large value However we b elieve part of the explanation

for this value lies in the low amplitude of variability of this star in as compared to the

0

light curve The photometric amplitude from the g data is  mmag

The data indicate a V band amplitude of  mmag Since the photometric

amplitude of Dor stars diminishes from A to A and presumably continues

to diminish at even longer wavelengths the combination of photometric noise with low

amplitudes might reasonably give a smaller WelchStetson index The biggest p eak in the

p ower sp ectrum of UVa yields a p erio d of days with a falsealarm probability

of If we assume the p erio d determined from the data is close to the true

p erio d and we also assume that p erio d is stable we nd that the data also fold

reasonably well to the p erio d

It is p ossible that the true second p erio d of UVa is the one day alias of the value

1

given ab ove or P  d Similarly for UVa the one day alias of

2

the p erio d given ab ove  d might b e its true principal p erio d These values are

not unheard of for Dor stars eg BS Zerbi et al Only a multilongitude

photometric campaign or extensive singlesite photometry over the course of a full season

could decide the matter

We feel condent that we have identied two Dor candidates in M We call these

stars candidates not bona de Dor stars b ecause we have no sp ectroscopic evidence ie

radial velocity andor line prole variations to prove conclusively that these two stars are

nonradial pulsators The evidence to date suggests that the Dor phenomenon o ccurs in

young stars Krisciunas et al and references therein While no Dor variables have

b een found in the Hyades age ab out Myr Perryman et al the much younger

Myr op en cluster NGC has several Dor candidates Zerbi et al M

has an age of ab out Myr Ianna Schlemmer Under the assumption that

IBVS

Figure Folded light curve of the M star UVa The V band data of dots and the

0

g band data of op en circles have b een folded with a p erio d of P days The data have

1

not b een prewhitened by the sinusoid with P days

2

Figure Folded light curve of the M star UVa The V band data of dots and the

0

g band data of op en circles have b een folded with a p erio d of days

IBVS

Dortype variability is just a phase in the life of an early Ftype star which ends when

its thin convection zone develops we have shown that the Dor phenomenon can p ersist

at least until such a star is Myr old

Acknowledgments We thank Hugh Harris of the U S Naval Observatory for arranging

the telescop e time Bruce Margon and the Sloan Digital Sky Survey pro ject for travel

supp ort and Lowell Observatory for accommo dations

References

Fukugita M Ichikawa T Gunn J E Doi M Shimasaku K Schneider D P

AJ

Ianna P A Schlemmer D M AJ

Krisciunas K Crowe R A Luedeke K D Rob erts M Monthly Notices

Royal Astr Soc

Krisciunas K Crowe R A IBVS No

Krisciunas K in Deubner FL ed New Eyes to See Inside the Sun and Stars

IAU Symp osium

Patten B M Krisciunas K in preparation

Perryman M A C et al AA

Welch D L Stetson P B AJ

Zerbi F M Mantegazza L Campana S Antonello E PASP

Zerbi F M et al Monthly Notices Royal Astr Soc

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

V Aql AN ECLIPSING CLASSICAL NOVA

R HAEFNER

UniversitatsSternwarte Scheinerstr M unchen Germany

V Aql Nova Aquilae exp erienced little observing attention The rather

incomplete outburst light curve eg PayneGaposchkin nevertheless allowed the

d

classication as a mo derately fast nova t After reaching the maximum brightness

of ab out mag photographic the system faded to mag Its distance amounts to

kp c eg Shafter From a sp ectrum taken ab out days after maximum the

expansion velocity was determined to b e  km s Sanford Based on the

presence of Ne I I I and Fe VI I lines in this sp ectrum Della Valle and Livio suggest

this nova to b e a member of the HeN class Further information eg co ordinates nding

chart literature may b e found in the catalogues published by Duerb eck or Downes

et al

The present photometric observations were obtained in August using the CCD

camera on the m Dutch telescop e at the Europ ean Southern Observatory Since the

star app eared quite faint  mag the measurements were p erformed in integral light

Table gives the observing log

Table Journal of observations Start is the time for the midp oint of the rst exp osure The observation

interval includes also gaps due to any interruption of the exp osure series

Date Start Interval Int Time Frames Obs

UT h min No Run

Aug

Aug

Dierential instrumental magnitudes were derived relative to nearby comparison stars

on the same CCD image Fig presents the resulting light curve obtained during the

rst night run Two eclipses depth  mag duration  min ab out hours

apart are easily recognizable Also shown are the measurements of a comparison star of

comparable brightness The larger scatter in the V Aql data hints at ickering activity

in the nova system Two further eclipses could b e recorded during the second night run

when the system was  mag brighter Further the eclipse proles had changed to

a somewhat shallower shap e All this indicates that V Aql was probably met at the

b eginning of a dwarf nova outburst a b ehaviour shared with some further classical novae

Unfortunately the data of the second night suer from worse meteorological conditions

resulting in a larger scatter After allowing for the mag dierence the combined data

IBVS

Figure The light curve of V Aql top compared with a constant star b ottom The

measurements were obtained on August

Figure The phased light curve of V Aql based on an orbital p erio d of hours Op en circles

data of run lled circles data of run

IBVS

set was sub jected to a p erio dogram analysis yielding an orbital p erio d of 

hours Fig shows the resulting phase diagram The large scatter during the eclipse

phase is due to the dierent eclipse proles and the enhanced scatter of run

The present data set do es not allow to derive more detailed parameters but it is su

cient to demonstrate the eclipse phenomenon in the V Aql system

References

Della Valle M Livio M ApJ

Downes RA Webbink RF Shara MM PASP

Duerb eck HW Space Sci Rev Nos

PayneGaposchkin C The Galactic Novae NorthHolland Publ Co Amsterdam

Sanford RF PASP

Shafter WA ApJ

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

THE DUST SHELL AROUND SAKURAIS OBJECT

T KIPPER

Tartu Observatory Toravere Estonia email tkaaiee

In our recent pap er Kipp er Klo chkova we analysed the sp ectra of the b orn

again giant Sakurais ob ject V Sgr whose evolution has b een extraordinarily rapid

We found that the eective temp eratures of the ob ject derived using sp ectral and photo

metric metho ds were quite consistent until March Later results diverge noticeably

The natural explanation for that is the increased circumstellar reddening and an extra

radiation from hot dust clouds as the star starts to show R CrBtype brightness drops

In this note we try to mo del this situation

The most comprehensive photometric data for June September and Octob er of

in U B V J H K LM colours were obtained from Arkhip ova et al Further data for

May in JHK were taken from Kamath Ashok and from the nearIR

sp ectrum gures of Eyres et al for April and July Shorter wavelength data

U B V Ri for April were taken from Duerb eck et al For dereddening the

E B V Duerb eck Benetti and for the ux calibration the zero p oint

uxes by Straizys were used The derived uxes are plotted in Fig As could

b e seen the data for nearIR deviate from each other quite noticeably This reects b oth

the large observation errors and the variability as the plotted data cover the half a year

time span

For mo delling the dust shell the publicly available co de DUSTY developed by Ivezic

Nenkova Elizur was used

For the input radiation from the central star the mo del sp ectra of Hdecient stars

were used Particularly for June and later we chose the mo del with T K

e

log g and CHe This was the mo del giving the b est t for the C bands in

sp ectra of Sakurais ob ject We have earlier found that the line sp ectrum had not

changed from Kipp er Klo chkova With assumed stellar mass of M

this corresp onds to log LL and R R



According to Zubko the most probable grain type acting in R CrB stars en

velopes are the graphite grains We used the optical prop erties of graphite grains by

Draine Lee In the course of mo delling we found that only single size grains

with radii around a  m allow to explain UBV observations of This is in

accord with Zubkos ndings that in the case of R CrB stars the size distributions

of dust grains have p eaklike form with typical sizes  m The constant dust

density in quite narrow shell thickness RR was adopted as the shell formed

in

during very short time

The dust temp erature T at the inner shell b oundary R was estimated from the

d in

observed sp ectral shap e and the lo cation of the p eak in nearIR region

IBVS

Figure Mo delling of circumstellar dust shell around Sakurais ob ject in Triangles Arkhip ova

et al for June diamonds ibid for September and Octob er asterisks Duerb eck et al

for April squares Kamath Ashok for May slanted crosses Eyres et al for March

crosses ibid for July The mo del sp ectra for June and July of are plotted with lines full line

total emerging ux dotted line contribution of the attenuated input radiation dashed line

contribution of the scattered radiation dashdotted line dust emission and dashdotdot line input

stellar photospheric sp ectrum

Figure The same as in Fig but the mo del sp ectra are plotted for April

IBVS

Figure Mo delling of circumstellar dust shell around Sakurais ob ject in and Triangles

Jacoby De Marco and Kaeu nearIR for June crosses Lynch et al for

March asterisks Jacoby for March Full line mo del total ux for March July

dashed line mo del ux for March

In that way for June and July of the following mo del was found visual optical

depth dust temp erature T R K inner radius of dust shell R

V d in in

R This mo del is plotted also in Fig In this mo delling the data by Arkhip ova et



al was given the highest weight

For April higher stellar temp erature T K smaller grain size a

e

m visual optical depth and rather high dust temp erature T K

V d

at R R were needed Fig The sp eed of the changes in the envelope parameters

in 

b etween these two dates is in the order of the timescale of gas acceleration found by

Fadeyev for R CrB dust envelopes

For the autumn of the mo del with spherical distribution of dust is imp ossible

as b oth optical and nearIR ux have risen The t is p ossible only if the luminosity of

the star was higher by ab out or there was a hole in dust towards the observer with

smaller extinction It should b e noted that according to AAVSO data the observed V

m

magnitudes vary rather erratically up to

In the star suered deep er brightness drops At the end of February the weakening

m

in V amounted to but the star almost recovered by the end of July when another much

deep er weakening started For the rst weakening the photometry by Jacoby De Marco

Kaeu and Lynch et al is plotted in Fig These observations

could b e approximated with the mo del having T K In this case in

V d

addition larger grains up to a m with standard IS distribution na / a and

larger relative thickness of the shell RR are needed Inclusion of larger grains

in

allows to mo del much atter output sp ectrum at the shorter wavelengths Larger relative

thickness gives b etter t in nearIR region The luminosity of the star should b e higher

by compared to July

The weakening which started in July has not yet stopp ed and by March

IBVS

the star was already as weak as V Jacoby These last data could b e

approximated with the mo del having and T not higher than K The

V d

colour alone corresp onds to a blackbo dy with temp erature of K Jacoby

This very deep and longlasting minimum indicates that Sakurais ob ject could share the

fate of another nal helium shell ash star V Aql which after four years of fadings and

brightenings disapp eared from the sky Clayton De Marco

The presented mo dels follow from very crude approximations The state of the system

is not steady but highly dynamical The outpus of dust are probably related to a

pulsational cycle of the central star This means that the input stellar radiation rapidly

changes The gas in which the dust grains condense is ejected rather in cones with semi



angle of ab out Feast than in spherical symmetry Nevertheless such mo delling

allows to explain why the eective temp eratures of the star determined from colours

and sp ectral data do not coincide and the sp ectral energy distribution of the system for

and later could b e explained with the constant eective temp erature of central star

T K

e

Acknowledgements The work on this note was supp orted by Estonian Science Founda

tion grant We have used and acknowledge with thanks the data from the AAVSO

International Database

References

Arkhip ova VP Esip ov VF Noskova RI et al Astron Lett

Clayton GC De Marco O AJ

Draine BT Lee HM ApJ

Duerb eck HW Benetti S ApJ L

Duerb eck HW Benetti S Gautschy A et al AJ

Eyres SPS Evans A Geballe TR et al MNRAS L

Fadeyev YuA MNRAS

Feast MW In Hydrogen Decient Stars eds Hunger K Schonberner D

Rao NK Reidel Dordrecht Holland

Ivezic Z Nenkova M Elizur M User Manual for DUSTY University of Ken

tucky

Jacoby G De Marco O IAU Circ No

Jacoby G IAU Circ No

Kaeu HU it IAU Circ No

Kamath US Ashok NM MNRAS

Kipp er T Klo chkova VG IBVS No

Lynch DK Russell RW Rice CJ IAU Circ No

StraizysV Multicolor Stellar Photometry Mokslas Publ Vilnius

Zubko VG MNRAS

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

BV PHOTOMETRY OF SX Phe BLUE STRAGGLERS

IN THE GLOBULAR CLUSTER NGC

JENNWOOD CHEN T MICHAEL CORWIN

UNC Charlotte Charlotte NC USA email mcorwinunccedu

Name of the ob ject

Blue stragglers NH NH NH NH NH NH in the globular cluster

NGC

Equatorial co ordinates Equinox

h m  0

RA DEC

Observatory and telescop e

The images were obtained with the No meter telescop e at Kitt Peak National

Observatory

Detector The  TI CCD with a pixel scale of arcsec

and the  TKA CCD with a pixel scale

of arcsec

Filters The Harris B and V lters were used with exp osure times

of s for the V frames and s for the B frames

Comparison stars Four stars in the eld were selected as lo cal magnitude

standards for relative photometry and

Buonanno et al

Transformed to a standard system UBV

Standard stars eld used Twentynine standard stars select

ed from Landolt with a

range in B V from to

mag were observed

Availability of the data

Through IBVS Website as ttxt ttxt ttxt ttxt

ttxt and ttxt

Type of variability SX Phe

IBVS

Remarks

We present a new photometric study of the six SX Phe blue stragglers in NGC

discussed by Nemec et al The images used in this study were ob

tained during May May April June and June The

raw data frames were pro cessed and reduced following standard pro cedures using

ALLSTAR in DAOPHOTX in IRAF The resulting ephemerides for maxima are

NH day ep o ch  days NH day ep o ch

 day NH day ep o ch  days

NH day ep o ch  day NH day ep o ch

 day and NH day ep o ch 

day

The light curves are for the B data The lled squares are data op en squares

are data lled triangles are data op en triangles are data and lled

circles are data The nding chart is published in Nemec and Harris

Figure Figure

IBVS

Figure Figure

Figure Figure

References

Buonanno R Buscema G Corsi C Iannicola G and Fusi Pecci F AAS

Landolt A AJ

Nemec J Nemec A and Lutz T AJ

Nemec J and Harris H ApJ

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN



BD A NEW UU HERCULIS VARIABLE

GLENN GOMBERT

Yorkshire Place Dayton OH USA glenginnetcom

Name of the ob ject



BD PPM GSC

Equatorial co ordinates Equinox

h m s  0 00

RA DEC J

Observatory and telescop e

Dayton TASS MkI I I camera system three CCD cameras each using mm f

lenses op erated serially in driftscan timedelay integration mo de

Detector Ko dak KAF arcsecpxl

Filters Johnson V

Transformed to a standard system Johnson V

Standard stars eld used First order transformation co e

cients were calculated using Lan

dolt standard stars in the Declina

 

tion zone to Nightly

zero p oints were set with Tycho

stars present in each image Per

observation internal uncertainties

m m

are exp ected to b e at

the magnitude of the variable An

analysis of the photometric accu

racy for a larger dataset has b een

p erformed by Richmond

Availability of the data

Through IBVS Website as ttxt

Type of variability SRd p ossibly UU Herculis type

IBVS

Remarks



BD was found to b e variable in data taken with the Dayton Ohio TASS

MkI I I camera system Gombert Dro ege The star is not present in the

Combined General Catalogue of Variable Stars GCVS Kholop ov et al

The star was observed times b etween UT dates July and Octob er

During this interval the star showed a welldened p erio dicity of days

The Tycho B V color of the star corrected to the standard system is 

This combined with the smallamplitude sawtoothshap ed lightcurve suggests the

star is of the UU Herculis type This is a rare class of highlatitude Ftype sup er

giants exhibiting sometimes varying mo des of pulsation but whose fundamental

characteristics are enigmatic cf Klo chkova et al Fernie Seager A

p erio d of ab out days more characteristic of UU Herculis type variables could

not b e established from the data collected to date

Acknowledgements

I would like to thank Michael Richmond Ro chester Institute of Technology for his

help and advice in preparing this rep ort and for preparing Figure I would like to

thank Brian Ski of Lowell Observatory for his help in determining a preliminary

classication for this new variable as well as reformatting this pap er for publication



Figure Photometry of BD phased for a p erio d of days

References

Fernie J D and Seager S Publ Astron Soc Pac

Gombert G J and Dro ege T R Sky Telescope No February

Henden A A and Kaitchuck R H Astronomical Photometry WillmannBell

Richmond

Kholop ov P N et al Combined General Catalogue of Variable Stars edition

Moscow httpvizierustrasbgfrcgibinVizieRsourceIIA

Klo chkova V G Panchuk V E and Chentsov E L Astron Astrophys

Richmond M W TASS Technical Note An Analysis of Dayton TASS Data

Reduced With Flatcomp Program httpaLritedutasstechnotestnhtml

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

CCD PHOTOMETRY OF V CASSIOPEIAE

PETR MOLIK MIROSLAV BROZ MAREK WOLF

Astronomical Institute Charles University Prague CZ Praha V Holesovickach Czech Republic

Email PMolikvuppcz miroslavbrozusanet wolfmboxcesnetcz

Name of the ob ject

V Cassiop eiae CSV GR GSC FL

Equatorial co ordinates Equinox

h m s  0 00

RA DEC J

Observatory and telescop e

Hradec KraloveObservatory Czech Republic m Newtonian telescop e

Detector SBIG ST CCD camera

Filters None

Comparison stars GSC

Check stars GSC

Transformed to a standard system No

Availability of the data

Through IBVS Website as ttxt

Type of variability EA

Remarks

New times of minimum light HJD HJD New light

elements

d

Pri Min HJD  E

 

O C diagram with resp ect to the new elements is plotted in Fig corresp onding

times of minima are available in electronic form through IBVS Web site

Our observations suggest in accordance with the previous photo electric measure

ments by Zhang et al that V Cas should b e classied as a short

p erio d Algol The depth of primary and secondary minima of V Cas are equal

within the observational errors therefore the choice of reference ep o ch in the ab ove given elements is arbitrary

IBVS

Figure O C diagram of V Cas The individual photo electric and CCD observations are

denoted by dots the photographic measurements by circles and visual estimations by triangles

References

Zhang JT Zhang RX Li CS Zhai DS Inf Bull Var Stars No

Zhang RX Zhang JT Li QS Zhai DS Acta Astron Sinica

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

PHOTOELECTRIC MINIMA OF SELECTED ECLIPSING BINARIES

BAV MITTEILUNGEN NO

FRANZ AGERER JOACHIM HUBSCHER

Bundesdeutsche Arb eitsgemeinschaft f urVeranderliche Sterne eV BAV Munsterdamm D Berlin

Germany

In this th compilation of BAV results photo electric observations obtained in the

years and are presented on variable stars giving minima and maxima

All moments of minima and maxima are helio centric The errors are tabulated in col

umn  The values in column O C are determined without incorp oration of nonlinear

terms The references are given in the section Remarks All information ab out photome

ters and lters are sp ecied in the column Rem The observations were made at private

observatories The photo electric measurements and all the lightcurves with evaluations

can b e obtained from the oce of the BAV for insp ection

Table Eclipsing binaries

Variable Min JD  Obs O C Fil Rem

RT And QU GCVS V

QU GCVS V

QU s GCVS V

AA And AG GCVS BV

AB And ATB s GCVS

BL And MS s GCVS

KN And MS BAVR

EK Aqr KI GCVS

EL Aqr KI GCVS

OO Aql QU s GCVS V

V Aql KI GCVS

V Aql AG BAVM BV

V Aql KI s BAVR

V Aql KI BAVM

GSC Aql QU Ir

RX Ari KI GCVS I

EM Aur FR s GCVS

HU Aur MS GCVS

IM Aur AG GCVS BV

AG GCVS BV

KO Aur AG GCVS BV

V Aur MS

MS

MS

TY Bo o MS BAVM

VW Bo o KI BAVR

XY Bo o AG s GCVS BV

AG GCVS BV

CK Bo o KI s GCVS

KI GCVS

IBVS

Table cont

Variable Min JD  Obs O C Fil Rem

FF Cnc FR BAVM

FR s BAVM

FR BAVM

FR s BAVM

BO CVn AG BV

XZ CMi KI GCVS

YY CMi ATB s GCVS

AK CMi KI GCVS

KI GCVS

AG GCVS BV

AM CMi ATB GCVS

BH Cas AG

AG

AG

DZ Cas AG GCVS

EN Cas MS GCVS

MS GCVS

V Cas AG GCVS

AG GCVS

V Cas MS GCVS

MS GCVS

V Cas MS GCVS

V Cas MS GCVS

V Cas MS BAVM

V Cas AG s BAVM BV

WW Cep AG BAVM

AG BAVM

EG Cep DIE GCVS

DIE GCVS

DIE GCVS

DIE GCVS

DIE GCVS

DIE GCVS

DIE GCVS

OT Cep AG s GCVS

RW Cet KI GCVS

TT Cet KI s GCVS

TX Cet KI GCVS

KI GCVS

VV Cet KI s GCVS I

SS Com KI s BAVR

CC Com KI GCVS

NSV Com MS BAVM

MS BAVM

KR Cyg FR GCVS

FR s GCVS

FR GCVS

FR s GCVS

FR GCVS

V Cyg AG SAC BV

V Cyg FR s GCVS

FR GCVS

FR s GCVS

FR s GCVS

FR s GCVS

FR GCVS

FR s GCVS

FR s GCVS

FR GCVS

FR GCVS

IBVS

Table cont

Variable Min JD  Obs O C Fil Rem

V Cyg FR GCVS

FR s GCVS

FR s GCVS

FR GCVS

FR GCVS

V Cyg MS GCVS

V Cyg AG s GCVS

V Cyg MS GCVS

V Cyg AG BAVM

V Cyg AG GCVS

AG s GCVS

V Cyg FR GCVS

FR GCVS

FR GCVS

V Cyg AG s GCVS

V Cyg MS GCVS

V Cyg AG BAVM

V Cyg AG GCVS

TY Del KI GCVS

AV Del KI GCVS

DM Del KI GCVS

EX Del KI GCVS Ir

FZ Del KI GCVS

GG Del KI GCVS

BX Dra AG GCVS

AG GCVS

AG s GCVS

EF Dra AG BAVM BV

BV Eri KI s GCVS Ir

WW Gem QU GCVS Ir

QU GCVS V

YY Gem HSR GCVS

QU GCVS Ic

QU s GCVS Ic

EY Gem AG GCVS

GX Gem FR s GCVS

UX Her MZ GCVS

HS Her AG GCVS BV

V Her AG s BAVM

V Her AG BV

V Her MS

MS

MS

MS

MS

V Her AG BV

AV Hya KI GCVS Ir

EU Hya KI GCVS

VY Lac AG s GCVS BV

CN Lac MS s GCVS

MS s GCVS

FL Lac MS GCVS

MS GCVS

IM Lac AG s GCVS

AG GCVS

V Lac AG s BAV unp BV

UV Leo MS s GCVS

UX Leo KI BAVM

XY Leo KI GCVS

XZ Leo QU GCVS V

IBVS

Table cont

Variable Min JD  Obs O C Fil Rem

AL Leo MS BAVM

AP Leo KI GCVS

RT LMi MS GCVS

SW Lyn DIE GCVS

DIE GCVS

UZ Lyr HSR GCVS Ir

QU Lyr AG GCVS

V Lyr MS GCVS

MS GCVS

BO Mon KI GCVS Ir

V Mon MS GCVS

V Mon MS s GCVS

MS GCVS

MS s GCVS

MS s GCVS

MS GCVS

MS s GCVS

MS s GCVS

MS GCVS

V Mon KI s GCVS

MS s GCVS

MS GCVS

KI GCVS Ir

V Mon MS GCVS

V Mon MS

V Mon MS GCVS

KI s GCVS

V Mon MS GCVS

V Mon MS GCVS

Remarks

AG Agerer F Tiefenbach FR Frank P Velden MS Moschner W Lennestadt

ATB Achterberg Dr H Norderstedt HSR Husar Dr D Hamburg MZ Maintz G Bonn

DIE Dietrich M Radeb eul KI Kleikamp W Marl QU Quester W Esslingen

uncertain

s secondary minimum

photometer CCD  uncoated lter VIr

photometer EMI A lter V GG mm B BG mm GG mm

photometer ST lter V or Ir KG

photometer OESLcCCD without lter

photometer LC without lter

photometer pictor XT

BAVM BAV Mitteilungen No IBVS No

BAVM BAV Mitteilungen No IBVS No

BAVM BAV Mitteilungen No IBVS No

BAVM BAV Mitteilungen No IBVS No

BAVM BAV Mitteilungen No IBVS No

BAVM BAV Mitteilungen No IBVS No

BAVM BAV Mitteilungen No IBVS No

BAVM BAV Mitteilungen No IBVS No

BAVM BAV Mitteilungen No IBVS No

BAVM BAV Mitteilungen No IBVS No

BAVM nn BAV Mitteilungen No nn

BAVR BAV Rundbrief

BAVR BAV Rundbrief

BAVR BAV Rundbrief

BAV unp BAV unpublish ed

GCVS nn General Catalogue of Variable Stars th ed nn

SAC xx Ro cznik Astronomiczny No xx Krakow SAC

IBVS

From IBVS

Corrections to IBVS No

RT And instead of QU correct is

V Cyg AG

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

PHOTOELECTRIC MINIMA OF SELECTED ECLIPSING BINARIES

AND MAXIMA OF PULSATING STARS

BAV MITTEILUNGEN NO

FRANZ AGERER MICHAEL DAHM JOACHIM HUBSCHER

Bundesdeutsche Arb eitsgemeinschaft f urVeranderliche Sterne eV BAV Munsterdamm D Berlin

Germany

In this th compilation of BAV results photo electric observations obtained in the

years and are presented on variable stars giving minima and maxima

All moments of minima and maxima are helio centric The errors are tabulated in col

umn  The values in column O C are determined without incorp oration of nonlinear

terms The references are given in the section Remarks All information ab out photome

ters and lters are sp ecied in the column Rem The observations were made at private

observatories The photo electric measurements and all the lightcurves with evaluations

can b e obtained from the oce of the BAV for insp ection

Table Eclipsin g Binaries

Variable Min JD  Obs O C Fil Rem

V Oph KI GCVS

V Oph KI GCVS

KI GCVS

V Oph KI GCVS

DZ Ori MS GCVS

MS GCVS

ER Ori KI s GCVS

KI GCVS I

FH Ori KI GCVS

KI GCVS I

FR Ori KI GCVS

FT Ori QU GCVS Ir

FZ Ori KI s GCVS Ir

GU Ori FR

FR

FR

V Ori KI s GCVS

AG GCVS BV

U Peg KI s GCVS I

AT Peg KI GCVS

BB Peg KI s GCVS

CC Peg AG GCVS

DO Peg KI GCVS

EU Peg MS GCVS

EY Peg AG

AG V

GH Peg KI GCVS I

HW Per MS s GCVS

MS GCVS

IBVS

Table cont

Variable Min JD  Obs O C Fil Rem

KL Per AG V

AG

V Per AG BAVM BV

AG s BAVM BV

V Per MS GCVS

V Per AG BAVM BV

V Per AG s IBVS BV

UV Psc KI GCVS

CU Sge KI GCVS

DK Sct KI GCVS

BI Ser AG GCVS

CC Ser AG s GCVS BV

Y Sex HSR BAVR

KI s BAVR

RZ Tau KI GCVS

KI s GCVS

KI s GCVS Ir

CU Tau MS GCVS

MS s GCVS

AG s GCVS

GR Tau AG s BAVR BV

KI BAVR I

QU BAVR V

V Tau MS

MS

KI I

X Tri HSR GCVS V

UY UMa AG GCVS

AG GCVS

AG s GCVS

AG s GCVS

AW Vir KI s GCVS

AZ Vir KI s GCVS

BH Vir KI GCVS

GR Vir KI s GCVS

HW Vir HSR Ir

KI

KI

KI

QU

QU

HI Vul AG GCVS

Table Pulsating stars

Variable Max JD  Obs O C Fil Rem

SW And PS BAVM

ATB BAVM

XX And ATB SAC

GP And ATB GCVS

KI GCVS Ir

OV And ATB MVS

BR Aqr KI GCVS I

CP Aqr KI GCVS

CY Aqr KI GCVS Ir

KI GCVS Ir

AA Aql KI BAVM

V Aql KI GCVS Ir

RV Ari MAR GCVS

MAR GCVS

IBVS

Table cont

Variable Max JD  Obs O C Fil Rem

RW Ari HSR GCVS

SY Ari KI Ir

TZ Aur ATB GCVS

ATB GCVS

RS Bo o ATB BAVR

TW Bo o HSR GCVS

UU Bo o HSR GCVS

UY Bo o HSR SAC Ir

HSR SAC Ir

YZ Bo o MZ GCVS

CG Bo o MS

CM Bo o QU BAVM

QU BAVM

HSR BAVM

BK BAVM

CQ Bo o QU MVS

HSR MVS Ir

BK MVS

CS Bo o HSR IBVS Ir

BK IBVS

AH Cam QU GCVS Ir

HSR GCVS

VZ Cnc KI GCVS

RZ CVn KRW ZAU GCVS

KRW ZAU GCVS

KRW ZAU GCVS

X CMi BK BAVR

Y CMi PS GCVS

HU Cas AG

GSC Cas MS

MS

MS

RR Cet KI GCVS Ir

RZ Cet KI GCVS I

S Com HSR SAC

ATB SAC

U Com PS GCVS

RY Com BK GCVS

ST Com ATB GCVS

SZ CrB MS GCVS

MS GCVS

XZ Cyg HSR BAVM Ir

DX Del KI GCVS

RT Equ PS GCVS

RX Eri PS GCVS

BK Eri KI GCVS Ir

SZ Gem QU GCVS V

QU GCVS V

KV Gem KI GCVS Ir

VX Her ATB BAVR

DY Her KI GCVS

RR Leo ATB GCVS

PS GCVS

SS Leo PS GCVS

MAR GCVS

ST Leo PS GCVS

HSR GCVS

SW Leo FR GCVS

WW Leo PS GCVS

TV Lib KI GCVS

IBVS

Table cont

Variable Max JD  Obs O C Fil Rem

CN Lyr HSR BAVR Ir

CM Ori HSR GCVS

VV Peg KI GCVS

BF Peg HSR GCVS

HSR GCVS

HSR GCVS

BP Peg HSR GCVS Ir

KI GCVS

DH Peg HSR GCVS Ir

KI GCVS I

DY Peg ATB GCVS

KI GCVS I

ATB GCVS

SS Psc ATB GCVS

AN Ser KI GCVS

AR Ser KI GCVS

CW Ser KI GCVS

DY Ser KI GCVS

RV UMa HSR GCVS

AE UMa MAR GCVS

ST Vir BK GCVS

UU Vir KI GCVS

AF Vir KI GCVS

AT Vir BK GCVS

AV Vir HSR GCVS Ir

BC Vir KI GCVS

FU Vir MS GCVS

Remarks

AG Agerer F Tiefenbach MAR Martignoni M Busto Arsizio I

ATB Achterberg Dr H Norderstedt MS Moschner W Lennestadt

BK Birkner C Hagen MZ Maintz G Bonn

FR Frank P Velden PS Paschke A Rueti CH

HSR Husar Dr D Hamburg QU Quester W Esslingen

KI Kleikamp W Marl ZAU Zaunick H Radeb eul

KRW Krawietz A Kurort Hartha

uncertain

s secondary minimum

photometer CCD  uncoated lter VIr

photometer EMI A lter V GG mm B BG mm GG mm

photometer Cryocam A without lter

photometer ST lter V or Ir KG

photometer OESLcCCD without lter

photometer LC without lter

BAVM BAV Mitteilungen No IBVS No

BAVM BAV Mitteilungen No IBVS No

BAVM nn BAV Mitteilungen No nn

BAVR BAV Rundbrief

BAVR BAV Rundbrief

BAVR BAV Rundbrief

BAVR BAV Rundbrief

BAVR BAV Rundbrief

BAVR BAV Rundbrief

GCVS nn General Catalogue of Variable Stars th ed nn

SAC xx Ro cznik Astronomiczny No xx Krakow SAC

IBVS xxxx Information Bulletin on Variable Stars No xxxx

MVS xx xxx Mitteilungen uber Veranderliche Sterne xx xxxx Sonneb erg

IBVS

From IBVS

Correction to IBVS No

UY UMa instead of AG correct is

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

ON THE ORBITAL PERIOD CHANGES OF AK HERCULIS

1 1 1 1

H ROVITHISLIVANIOU A KRANIDIOTIS E FRAGOULOPOULOU N SERGIS

2

P ROVITHIS

1

Section of Astrophysics Astronomy and Mechanics Dept of Physics University of Athens Panepistimio

p olis GR Zografos Athens Greece email elivanccuoagr

2

Astron Inst National Obs of Athens PO Box Athens Greece email rovithisastronoagr

AK Her is a contact eclipsing binary of W UMatype and the brighter comp onent of the

double star ADS Its companion is ab out magnitudes fainter than the eclipsing

00 

pair and lies very close to it at a distance of in p osition angle

The variability of AK Her was rep orted by Pickering and the system has b een

observed photo electrically many times for details see at Tunca et al and the refer

ences therein The system exhibits variable light curve and an obvious OConnell eect

Besides AK Her is an Xray source Cruddace Dupree

So far many studies have b een made concerning its p erio d variations and the detected

p erio dicities are extended from to years This is mainly due to the available ob

servational material at the time of analysis and secondly to the fact that the search for

p erio dicities was based on the O C diagram which dep ends on the ephemeris used So

Schmidt Herczeg found a p erio dicity of yr Woo dward Wilson of

yr Barker Herczeg of yr Glownia of and Tunca et al

of years In this rep ort b esides the unpublished times of minimum light of

AK Her that we present we also examine its orbital p erio d changes which was found not

to follow the sinusoidal variation prop osed some years ago

Our photo electric observations of AK Her were carried out during nights in

in and in with the m Cassegrain reector at the Kryonerion Astronomical

Station of the Athens National Observatory Greece Standard B and V lters and a two



b eam multimode nebularstellar photometer were used The stars BD and



BD were used for comparison and checking resp ectively and reduction of the

observations was made in the usual way Hardie Henden Kaitchuk The

derived new times of minimum light are presented in Table the successive columns

of which give the Hel JD the type of minimum and the O C where the Cs were

computed using the Kwee van Woerden metho d they are the mean values from

the B V observations and Woo dwards light elements were used

d

Min I  E

In order to construct the O C diagram of AK Her Fig Tuncas et al list of minimum light was used together with our data Table and the list was completed

IBVS

Table The times of minimum light of AK Her as derived from our photo electric observations

Hel JD Min Ep o ch O C

Type days

I

II

I

II

II

I

II

II

II

with up to date data which are given in Table In Fig the b est tted p olynomial for

details see Kalimeris et al used to describ e the data is presented by the heavy

continuous line while the sinusoidal term found by Tunca et al is denoted by the

dashed line

The real orbital p erio d variation P E and its rate of change were also computed

as it is describ ed by Kalimeris et al and from the Fourier sp ectrum of the

P E function two p erio dicities were detected viz  yr and  yr with

amplitudes of  sec and  sec resp ectively The rst p erio dicity is

close to this of yr found by Barker Herczeg and to that of yr found by

Tunca et al but since it corresp onds to the time interval for which observational

data exist it might not b e true

From the present analysis which includes the most recent available data it is shown

Fig that the orbital p erio d of AK Her does not fol low a sinusoidal variation This

could not b e detected from the observational material available at the time of the previous

analyses and shows clearly that the p erio d variations cannot b e predicted As regards the

second p erio dicity of yr it had not b een detected b efore but since it is half of the

long one more data are needed to assure its existence

Acknowledgements This work was partly nancial supp orted by Athens University

grant no

IBVS

Table Photo electric times of minimum light of AK Her from the literature

Hel JD O C Ep o ch Reference

days

AA

BAC

BAC

BAV No

BAV No

BAV No

BAC

AN

BAC

BAC

BAC

BAC

AN

AN

BBSAG

IBVS

IBVS

IBVS

IBVS

IBVS

IBVS

IBVS

IBVS

IBVS

IBVS

IBVS

IBVS

IBVS

IBVS

BBSAG

IBVS

IBVS

IBVS

IBVS

IBVS

Figure The O C diagram of AK Her and the b est tted p olynomial continuous line The

sinusoidal variation dashed line prop osed by Tunca et al is also given

References

Barker LA Herczeg TJ PASP

Cruddace R G Dupree AK ApJ

Glownia Z IBVS No

Hardie RH Stars and Stellar Systems Vol I I Astronomical Techniques WA

Hiltner ed Univ of Chicago Press Chicago p

Henden AA Kaitchuk RH Astronomical Photometry Chapter p Van

Nostand Reinhald Co Inc

Kalimeris A RovithisLivaniou H Rovithis P AA

Kalimeris A Mitrou C Doyle Antonopoulou E RovithisLivaniou H AA

Kwee KK van Woerden H Bull Astron Inst Neth

Pickering EC Harvard Circ No

Schmidt H Herczeg T Zf Ap

Tunca Z Keskin V Acan CM Evren S Ibanoglu C ApSS

Woo dward FJ Wilson RF ApSS

Woo dward FJ Harvard Circ No

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

DISCOVERY OF THE OPTICAL VARIABILITY

RXS J OF THE STAR GSC

1 2 1

RM ROBB DD BALAM AND R GREIMEL

1

Guest User Canadian Astronomy Data Centre which is op erated by the Herzb erg Institute of Astrophysics

National Research Council of Canada

2

Guest Observer Dominion Astrophysical Observatory which is op erated by the Herzb erg Institute of As

trophysics National Research Council of Canada

Climenhaga Observatory Dept of Physics and Astronomy University of Victoria Victoria BC Canada

VW P Internet robbuvicca cosmosuvvmuvicca greimeluvastrophysuvicca

The star RXS J H unsch et al GSC Jenkner et al

G Giclas et al was found to have signicant Xray emission in a

survey by the ROSAT satellite Bade et al Beers et al discovered the star

to have Ca HK lines in emission It was classied as an M star by Henry et al

with an apparent magnitude of V and B V as measured by Weis

As part of a search for radial velocity variations of nearby M dwarfs Delfosse et al

observed the hydrogen lines to b e in emission measured the radial velocity to b e kms

with a v sin i of kms and concluded that the star had a space motion consistent with

it b eing a member of the young disk at a distance of  p c

1 3 h 3 2 m 1 0 s 1 3 h 3 2 m 1 3 h 3 1 m 5 0 s 1 3 h 3 1 m 4 0 s + 2 9 o 2 0 ’

+ 2 9 o 1 8 ’

139 658 711 + 2 9 o 1 6 ’

360

o + 2 9 1 4 ’ 107 987

1 3 h 3 2 m 1 0 s 1 3 h 3 2 m 1 3 h 3 1 m 5 0 s 1 3 h 3 1 m 4 0 s

Figure Chart of our observed eld lab eled with the GSC numbers from Region

IBVS

Table Stars observed in the eld of GSC

RA Dec Cat R

ID No

J J Mag Mag

RXS J

h m s  0 00

GSC 

h m s  0 00

GSC

h m s  0 00

GSC 

h m s  0 00

GSC 

h m s  0 00

 GSC

h m s  0 00

GSC 

The eld of stars observed with the automated m telescop e is plotted in Figure

The data were reduced in a fashion identical to that describ ed in Robb et al

The stars identication numbers co ordinates and magnitudes from the Hubble Space

Telescope Guide Star Catalog GSC Jenkner et al are included in Table The

standard deviation of the dierential magnitudes from p oint to p oint during a night ranged

m m

from for bright stars on a go o d night to for the faintest star on p o or nights

This measures the precision of the brightness variations on the time scale of a few minutes

We measure the night to night precision of the data by calculating the standard devia

tion of the nine nightly means The run means and standard deviations are tabulated in

The high precision of these data Table as R in the sense of star minus GSC

minus can b e seen from the standard deviation of the R in the sense of GSC

m

GSC which is and shows that these two stars are constant at this level

has a large standard deviation making us susp ect of precision The star GSC

had obvious it of variability however our data are inconclusive The star GSC

m

variations of approximately p eak to p eak

−0.50

−0.48 ∆ R ∆ R ∆ R

−0.46

−0.44

−0.42

57.8 57.9 58.0 68.8 68.9 69.0 96.8 96.9 97.0 −0.50

−0.48 ∆ R ∆R ∆ B

−0.46

−0.44

−0.42

70.8 70.9 71.0 74.8 74.9 75.0 96.8 96.9 97.0

Figure Individual nights HJD data for RXS J

Examples of individual nights data are all plotted at the same scales in Figure with

the B data shifted by The abscissa is the Julian Date and the

IBVS

rightmost plots were observed simultaneously on Julian Date The telescop e at

the University of Victoria was used to measure in the R and I lters and the m

telescop e of the National Research Council of Canada was used to observe the B data

m m

The light curve amplitude in B is double the amplitude in R which is

m

double the amplitude in I Neither the maxima nor minima were consistent in

brightness during a night Flares were observed at HJD and

indicating that this is a UV Ceti type star

The nine nights were searched for p erio dicity by tting a single sine curve of various

frequencies to the data In Figure we have plotted the RMS deviation of a p oint from

a single sine curve as a function of frequency

0.013

0.012

0.011 RMS Residual

0.010

0.009 7.5 8.0 8.5 9.0 9.5 10.0 10.5 11.0

Cycles per Day

Figure Periodogram for RXS J for

Thirteen times of maximum brightness were found using the metho d of Kwee and

van Woerden to b e HJD

I B and B The

last two observations were made in B lter and are not signicantly dierent from the

second last two which were made in R considering our uncertainty of approximately

d



The photometric p erio d and ep o ch of GSC are unambiguously determined to

b e

d d

HJD of Maxima  E

where the uncertainties in the nal digits are given in brackets

GSC R magnitudes Using this ephemeris the dierential GSC

of all the nights are plotted in Figure with dierent symbols for each of the nights Plots

at multiples of this p erio d yielded no improvement in the scatter From the variation in

the brightness of successive maxima and minima we susp ected a second p erio dicity would

b e found Therefore the b est tting sine curve was subtracted from the data and another

search for p erio dicities was p erformed No signicant p erio ds were found

Although we considered a pulsating mo del and a sup erhumper cataclysmic system

we susp ect that this variation is due to a hot sp ot whose pro jected area changes as the star

rotates The amplitude of the curves in B R and I are well t by a sp ot approximately

IBVS

Figure R band light curve of RXS J for

degrees in pro jected radius with a temp erature of times the surrounding photosphere

The variation in the brightness of the maxima and minima could b e caused by changes

in the size or temp erature of the sp ots Our rotation p erio d a radius of R and



the v sin i of Delfosse et al give an inclination of  for the axis of rotation

The quoted uncertainty do es not include a contribution from dierential rotation which

could b e signicant

Therefore we b elieve RX to b e a very rapidly rotating MVe star with

active regions generating an Xray bright corona and emission lines and a hot sp ot mo d

ulating the light curve For this star to rotate so rapidly we exp ect it to b e orbited by

a close companion and have b egun sp ectroscopic observations to lo ok for evidence of its

existence

References

Bade N Engels D Voges W Beckmann V Boller Th Cordis L Dahlem M Engl

hauser J Molthagen K Nass P Studt J Reimers D AA Sup

Beers T Bestman W and Wilelm R AJ

Delfosse X Forveille T Perrier C Mayor M AA

Giclas HL Burnham RJr Thomas NG Lowell Obs Bull

Henry T Kirkpatrick J and Simons D AJ

H unsch M Schmitt JHMM Sterzik MF and Voges W AA Sup

Jenkner H Lasker B Sturch C McLean B Shara M Russell J AJ

Kwee KK van Woerden H BAN

Robb RM Greimel R Ouellette J IBVS No

Weis EW AJ

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

May

HU ISSN

VARIABLE STARS NEAR V Aql Aql X

T J REYNOLDS J R THORSTENSEN AND N D SHERMAN

Dept of Physics and Astronomy Dartmouth College Wilder Lab oratory Hanover NH USA

email johnthorstensendartmouthedu

We monitored V Aql Aql X in the I band b etween June and using

the m telescop e at MDM observatory obtaining usable second exp osures

Results for Aql X itself were rep orted by Shahbaz et al we refer the reader to

that pap er for further instrumental detail Here we rep ort on variable stars serendipitously

detected in our arcmin square eld

Using the DAOPHOT implementation in IRAF we selected stars on one of our

b est images and measured magnitudes through p ointspread function tting on all the

images We used observations of Landolt standard star elds to transform the

magnitudes to approximate KronCousins I to an estimated accuracy of  mag

The measured stars ranged from  I  Not all stars were measurable on all

images b ecause of variations in centering and seeing After collating the measurements

automatically and adjusting the instrumental magnitudes to a common dierential scale

we searched for variables by plotting the standard deviation of each stars measurements

against the mean magnitude At I we examined stars with this degraded

to at I and nally to near our limit of I Light

curves of  candidate variables were examined by eye and correlated with the direct

Table Variable Stars

a a

number RA Dec I I P d Type

max min

h m s  0 00

EW

h m s  0 00

EW

h m s  0 00

EW

h m s  0 00

EW

h m s  0 00

EW

h m s  0 00

EW

h m s  0 00

EW

h m s  0 00

EW

h m s  0 00

EA

a

ICRS essentially J Referred to USNO A

IBVS

Figure Light curves

Figure Nightly light curves of the eclipsing variable Number

IBVS

00

Figure I band nding charts for the nine variable stars Each panel is square with north at the top and east to the left

IBVS

image in most cases the variations were found to b e spurious largely b ecause of varying

contributions from very bright stars or proximity to the edge of the eld

Nine variables proved to b e genuine and none of these app ear to b e catalogued In

eight of the nine stars the variations are p erio dic Their light curves are shown in Fig

Because the light curves app ear consistent with W UMa stars the plots and p erio ds are

constructed assuming two minima p er orbit The remaining variable star showed a single

dip consistent with an eclipse and Fig shows its light curve during four nights Table

summarizes the information ab out these variables the celestial co ordinates are derived

from a t to numerous USNO A catalog stars Monet et al and are estimated

00

accurate to  The p erio ds in Table should typically b e accurate to  d

given the length of the data stream Fig shows nding charts

We are clearly not sensitive to variable stars with p erio ds much longer than our week

long observation window but our census should b e fairly complete for shorterp erio d

variations

References

Landolt A AJ

Monet D et al USNOSA US Naval Observatory Washington DC

Shahbaz T Thorstensen J R Charles P A Sherman N D MNRAS

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

A SUSPECTED VARIABLE OBJECT IN THE FIELD OF C

CHULHEE KIM

Dept of Earth Science Education Chonbuk National University Chonju South Korea

kimastromoakchonbukackr

Equatorial co ordinates Equinox

h m s  0

RA DEC

Observatory and telescop e

BOAO Bohyun Astronomical Observatory m reector

Detector Thinned back illuminated TEK  chip

Filters B

Comparison stars See Figure

Check stars See Figure

Transformed to a standard system No

Availability of the data

Through IBVS Website as ttxt

Type of variability ZZ Ceti

Remarks

In order to monitor the intraday variability the blazar C was observed with the

BOAO Bohyun Astronomical Observatory m reector As a byproduct this

variable ob ject was found We carried out ap erture photometry via the APPHOT

program in the IRAF package in order to determine the dierential photometric

magnitudes The exp osure time was ab out ve minutes The light curve is similar

to that of the variable white dwarfs classied as ZZ Ceti stars

Acknowledgements

The present study was partly supp orted by the Korea Research Foundation Pro ject D

IBVS

Figure Finding chart of the new variable The blazar C is denoted by

Figure a light curve of the new variable b magnitude dierences b etween the comparison and check stars

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

GSC A NEWLY DISCOVERED VARIABLE STAR

R DIETHELM

BBSAG Rennweg CH Ro dersdorf Switzerland

Astronomisches Institut der UniversitatBasel Venusstrasse CH Binningen Switzerland

email diethelmastrouni basch

Name of the ob ject

GSC

Equatorial co ordinates Equinox

h m s  0 00

RA : DEC J

Observatory and telescop e

R Szafraniec Observatory Metzerlen Switzerland cm RC telescop e

Detector SBIG ST CCD camera

Filters None

Comparison stars GSC

Check stars GSC

Transformed to a standard system No

Availability of the data

Up on request

Type of variability Unknown

Remarks

In the course of an ongoing study aimed at securing the light curve and the el

ements of variation for the eclipsing binary DW Ori we found the nearby star

GSC GSC magnitude to b e variable with an amplitude of at

least mag While the observations secured during one night do not show vari

ability ab ove the accuracy of the photometry mag a brightening was found

during the interval covering days This leads us to conclude that GSC

probably b elongs to a class of slowly varying stars

Acknowledgements

Photometry at the R Szafraniec Observatory is supp orted by the Emilia GuggenheimSchnurr Foundation

IBVS

Figure CCD light curve of GSC

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN



THE RADIAL VELOCITY OF DOUBLEMODE CEPHEID BD

1 2 2 2 1

SV ANTIPIN NA GORYNYA ME SACHKOV NN SAMUS LN BERDNIKOV AS

1 1

RASTORGOUEV EV GLUSHKOVA

1

Sternberg State Astronomical Institute Universitetsky Ave Moscow Russia

2

Institute of Astronomy Russian Academy of Sciences Pyatnitskaya Str Moscow Russia



CEPBtype variability of BD was recently discovered by Antipin

The star was bright enough to include it in our programme of Cepheid radial velocity

measurements so the new variable b ecame the sixth b eat Cepheid in our observations

along with CO Aur TU Cas EW Sct V Sct and BQ Ser In we obtained

V measurements at the cm and m reectors of Simeiz Observatory equipp ed with the

r

correlation sp ectrometer Tokovinin Table contains HJD helio centric V values

r

and their internal rms errors The value of gammavelocity from these observations is

V  kms

Figure The phased radialvelocity variations See description in text

In Figure we present phased V curves for the elements taken from Antipin

r

d

JD  E fundamental mo de Fig ac and

max

d

JD  E rst overtone mo de Fig b d

max

Figures ab are based on original measurements Figures cd are constructed for devi

ations from the mean phased curve of the other oscillation from the rst overtone for

IBVS



Table Radial velocities of BD

HJD V kms HJD V kms HJD V kms

r r r

Fig c and from the fundamental mo de for Fig d additionally the frequency con

d

nected with nonlinear interaction of the two main mo des P P P

has b een whitened The rst overtone mo de strongly dominates in variations of radial

velocity as well as in light variations The semiamplitudes of V are K kms and

r

K kms

Using the mo dication of Balonas metho d describ ed in Sachkov we



derived the radius of BD from the radialvelocity measurements Table and

photo electric BVI measurements obtained in JD by one of the authors

LNB Two color indices B V and V I were used as indicators of the eective

temp erature the results from them are in excellent agreement and with low formal errors

 R from B V and  R from V I The resulting log R value is

in agreement with the value predicted from the p erio dradius relation derived by

Sachkov

The authors are very grateful to AA Tokovinin for p ossibility to observe with the

correlation sp ectrometer and to the administration of Simeiz Observatory This study

was partially supp orted by the Russian Foundation for Basic Research by the Council of

the Program for the Supp ort of Leading Scientic Schools and by the National Program

Astronomy

References

Antipin SV Inf Bul l Var Stars No

Balona LA MNRAS

Sachkov ME Inf Bul l Var Stars No

Tokovinin AA Soviet Astronomy

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

COORDINATES AND IDENTIFICATIONS

FOR SONNEBERG VARIABLES I

BRIAN A SKIFF

Lowell Observatory West Mars Hill Road Flagsta AZ USA email baslowelledu

This rep ort contains identications and accurate p ositions for variables discovered

by Homeister Most are shortp erio d variables in the constellation Hercules The

working metho ds were similar to previous lists eg Ski which involves comparing

the source charts against computerscreen plots of the GSC or USNOA star cata

logues with Digitized Sky Survey images and making bibliographic comparisons using

the Strasb ourg VizieR utility and SIMBAD

The list is divided into four tables as given by Homeister from diering plate mate

rial The tables show Sonneb erg serial numbers and GCVS designations in the rst two

columns An asterisk by the GCVS name indicates a note following the tables The star

p ositions are from either the ACT Urban et al or USNOA Monet et al

The source of the p osition is given in column s A USNOA T ACT Several

of the stars in Table have precise co ordinates previously published by de Martino et al

as part of the Yale southern prop ermotion program GSC names are given as

available A few new IDs with external catalogues are given in the remarks or the notes

Table Variables on southern skypatrol plates

Sonne GCVS RA Dec s GSC Remarks

S NSV A

S TU Phe T

S NSV T HD

S NSV A

S NSV A

S NSV A

S NSV T

IBVS

Table Variables in the Herculis astrograph eld

Sonne GCVS RA Dec s GSC Remarks

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A galaxy VI I Zw

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

IBVS

Table Variables in the Herculis Schmidt eld

Sonne GCVS RA Dec s GSC Remarks

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A quasar z

S V Her A

S V Her A IRAS

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A

S V Her A CCDM JA

Table Variables in highlatitude elds

Sonne GCVS RA Dec s GSC Remarks

S DI UMa A

S TZ Com A

S CV Vir A

Notes

NSV BPS CS SB

V Her star marked is not red

V Her assumed to b e the southeastern star of a pair

V Her assumed to b e the eastern star of a pair

References

de Martino R Ko cyla D Predom C and Wetherbee E IBVS No

Homeister C Astron Nach

Monet D Bird A Canzian B Harris H Reid N Rho des A Sell S Ables H

Dahn C Guetter H Henden A Leggett S Levison H Luginbuhl C Martini

J Monet A Pier J Riep e B Stone R Vrba F Walker R USNOA

US Naval Observatory Washington DC see also httpwwwusnonavymilpmm

Ski B A IBVS No

Urban S E Corbin T E and Wyco G L Astron J

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

COORDINATES AND IDENTIFICATIONS

FOR SONNEBERG VARIABLES II

BRIAN A SKIFF

Lowell Observatory West Mars Hill Road Flagsta AZ USA email baslowelledu

The lists b elow give accurate co ordinates for some designated and susp ected vari

ables in several elds describ ed by Homeister The working metho ds were similar

to previous lists eg Ski which involves comparing the source charts against

computerscreen plots of the GSC or USNOA star catalogues with Digitized Sky

Survey images and making bibliographic comparisons using the Strasb ourg VizieR util

ity and SIMBAD

The tables are arranged as previously divided by region as in Homeisters lists The

Sonneb erg serial number and the GCVS designations app ear in the rst two columns

An asterisk by the GCVS name indicates a note which app ear at the end of the tables

The p ositions are taken mostly from USNOA Monet et al for some bright

stars the ACT Urban et al is adopted and for a few crowded stars p ositions have

00

b een estimated  using largescale Digitized Sky Survey frames from the Go ddard

SkyView facility McGlynn et al The source of the p osition is co ded in column

s as follows A USNOA S SkyView T ACT Many of the NSV stars in

the  CMa eld have b een dealt with previously by Lop ez who gives accurate

co ordinates for southern NSV stars

I made the matchup with the GSC using VizieR and found the various IDs in the

Remarks and Notes using SIMBAD The IDs are listed only if they are new in the sense

of b eing either not present or not linked in the same entry in SIMBAD

A few stars defeated my attempts to identify them Given that some of the stars I did

0

nd have p ositions as much as in error it is likely that these lost ones have similar

errors of some kind

IBVS

Table h Persei eld

Sonne GCVS RA Dec s GSC Remarks

S KX Per A

S NSV A

S KY Per A

S KZ Per A

S LL Per A

S NSV A

S NSV A

S LM Per A

S LN Per A

S NSV not found

S LO Per A

S LP Per A

S LQ Per S

S LR Per A

Table North Galactic Pole elds

Sonne GCVS RA Dec s GSC Remarks

S BI UMa A

S AG UMa A

S AH UMa A

S BK UMa A

S AI UMa A

S AK UMa A

S CC UMa T IRAS

S AL UMa A

S AM UMa A

S AN UMa A

S BL UMa A

S AO UMa A FBS B

S AP UMa A

S BM UMa A

S AQ UMa A

S AR UMa A CSO

S BN UMa A

S AS UMa A

S BO UMa A

S BP UMa A

S AT UMa A

S AU UMa A

S BQ UMa A

S BR UMa A

S BS UMa A

S BV Leo A

S AV UMa A

S AT Leo A

S BT UMa A

S BU UMa A

S AY Leo A

S NSV A ID uncertain

IBVS

Table North Galactic Pole elds contd

Sonne GCVS RA Dec s GSC Remarks

S CD Leo A

S BI Leo A

S CE Leo A

S NSV A

S CG Leo A

S CH Leo A

S BO Leo A

S BP Leo A

S BS Leo A

S VX Com A

S BV Com A

S BW Com A

S WZ Com A

S NSV A

S CM Com A

S AC Com A BPS BS

S AD Com A

S CQ Com A

S CR Com A

S AF Com A

S AG Com A

S CU Com A

S NSV A

S CY Com A

S CZ Com A BPS BS

S AK Com A

S NSV A

S DI Com A

S AM Com A Ton

S DK Com A

S DM Com A

S AO Com A

S DO Com A

S DP Com A

S AP Com A

S DR Com A

S EH Com A

S AX Com S

S BC Com A

S BB Com A

S EQ Com A

S EU Com A

S FF Com A

S BL Com A

S BO Com A

S FL Com A

S BQ Bo o A

S BT Bo o A

S AP Bo o A

S AY Bo o A BPS BS

IBVS

Table Cygni eld

Sonne GCVS RA Dec s GSC Remarks

S NSV T IRAS

S V Cyg A

S NSV A

S V Cyg A

S NSV A

S V Cyg A IRAS

S BL Dra A

S V Cyg A IRAS

S V Cyg A

S V Cyg A

S V Cyg A

S BM Dra not found

S NSV T

S V Cyg A

S V Cyg A IRAS

S NSV A

S V Cyg A

S V Cyg A

S V Cyg A IRAS

S V Cyg A

S BN Dra A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A IRAS

S V Cyg A IRAS

S V Cyg A

S V Cyg A

S BP Dra A

S BQ Dra A IRAS

S V Cyg A

S BR Dra A

S NSV A

S V Cyg A

S V Cyg A

S V Cyg A IRAS

S V Cyg A

S V Cyg A

S NSV A

S GX Cep A

S V Cyg A

S V Cyg A

S V Cyg A

S GY Cep T IRAS

S NSV A

S V Cyg A

S NSV A

S V Cyg A

S V Cyg A

S V Cyg A

IBVS

Table Cygni eld contd

Sonne GCVS RA Dec s GSC Remarks

S NSV S

S V Cyg A

S V Cyg A IRAS

S V Cyg A

S V Cyg A

S NSV A

S NSV A

S V Cyg A

S NSV A

S V Cyg A IRAS

S V Cyg A

S V Cyg A

S NSV A

S NSV A

S V Cyg A

S V Cyg A

S NSV A IRAS

S V Cyg A IRAS

S V Cyg A

S NSV A

S NSV T

S NSV A

S HH Cep A IRAS

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A IRAS

S NSV A

S V Cyg A

S OW Cep A IRAS

S NSV A

S V Cyg A

S NSV A IRAS

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S NSV A

S V Cyg A

S V Cyg A

S NSV A

S V Cyg A

S V Cyg A

S NSV A

S V Cyg A

S V Cyg T

S HK Cep A

S V Cyg A

S V Cyg A

S FL Cep A

S FK Cep A

S OX Cep A

IBVS

Table  Geminorum eld

Sonne GCVS RA Dec s GSC Remarks

S V Ori not found

S V Ori A

S IW Gem A IRAS

S HR Gem A

S V Ori A

S V Ori A

S NSV A

S V Ori A

S V Ori A

S NV Gem A

S HU Gem A

S HV Gem A IRAS

S IY Gem not found

S HW Gem A

S NSV A IRAS



S NW Gem T BD

S NX Gem T IRAS

S HY Gem not found

S KM Gem A

S HZ Gem A

S I I Gem S

S IL Gem A

S IM Gem A

S NR Gem A

S IN Gem A

S IO Gem A

S KP Gem A

S KQ Gem A

S KR Gem A

S IP Gem A

S NSV A

S MP Gem A

S NS Gem A

S NT Gem A IRAS

Table Persei eld

Sonne GCVS RA Dec s GSC Remarks

S LU Per A

S LV Per S IRAS

S LW Per A IRAS

S LZ Per A IRAS

IBVS

Table  Canis Ma joris eld

Sonne GCVS RA Dec s GSC Remarks

S EI CMa A

S EK CMa A IRAS

S EL CMa A

S NSV A

S NSV A

S NSV A

S EM CMa A

S EN CMa A

S NSV A CGCS

S NSV A IRAS

S EO CMa A

S EP CMa A IRAS

S NSV A

S EQ CMa A

S EX CMa A

S ER CMa A

S NSV A

S NSV A

S NSV A IRAS

S NSV A

S ES CMa A

S NSV A

S ET CMa A

S NSV T

S NSV A

S NSV A

S NSV A

S EU CMa S p osition uncertain

S NSV A IRAS

S NSV A

S NSV T CSS

S NSV A IRAS

S NSV A

S NSV A

Table Northern winter elds

Sonne GCVS RA Dec s GSC Remarks

S NSV A

S NSV A

S NSV A

S NSV A merged pair on DSS

S NSV A

S NSV A

S V Ori A

S V Ori S IRAS

S IZ Aur A

S NSV A

S NSV A

S NSV A

S KL Aur A

S KM Aur A

S KN Aur S

S NSV A

IBVS

Notes

KM Aur northeastern star of a pair



KN Aur on northeast side of and very close to BD

EO CMa veried on POSSI prints

AG Com SS I I BPS BS

AX Com northwestern star of pair cf Meinunger

BO Com ID uncertain bluer star chosen

EU Com IRC IRAS

V Cyg southwestern star of a pair

V Cyg assumed to b e brighterwestern star of a pair

V Cyg assumed to b e northeastern star of a pair

V Cyg ID somewhat uncertain assumed to b e brighter star at chart lo cation

V Cyg IRAS probably corresp onds to the galaxy sup erp osed on

west side of star  p eak

V Cyg IRAS IRC

I I Gem IRAS probably applies b oth to this star and to the brighter

red star immediately west

MP Gem double p osition is for southern star

NW Gem also IRAS

NX Gem also IRC

CD Leo sup erp osed on faint galaxy

NSV southwestern star of a pair

NSV IRAS error ellipse very large so p ossibly includes other ob jects

NSV ID uncertain p osition is for northern star of a pair

NSV almost certainly the variable is mismarked on chart and the nearby

red star and IRAS source intended

NSV southern star of a pair

References

Homeister C Astron Nachr

Lop ez C E IBVS No

McGlynn T Scollick K and White N httpskviewgsfcnasagov see also

SkyView The MultiWavelength Sky on the Internet in McLean B J et al New

Horizons from MultiWavelength Sky Surveys IAU Symp osium No p

Kluwer

Meinunger I Mitt Verand Sterne

Monet D Bird A Canzian B Harris H Reid N Rho des A Sell S Ables H

Dahn C Guetter H Henden A Leggett S Levison H Luginbuhl C Martini

J Monet A Pier J Riep e B Stone R Vrba F Walker R USNOA

US Naval Observatory Washington DC see also httpwwwusnonavymilpmm

Ski B A IBVS No

Urban S E Corbin T E and Wyco G L Astron J

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

COORDINATES AND IDENTIFICATIONS

FOR SONNEBERG VARIABLES III

BRIAN A SKIFF

Lowell Observatory West Mars Hill Road Flagsta AZ USA email baslowelledu

The lists b elow give accurate co ordinates for over designated and susp ected vari

ables in several elds describ ed by Homeister The working metho ds were simi

lar to previous lists eg Ski which involves comparing the source charts against

computerscreen plots of the GSC or USNOA star catalogues with Digitized Sky Sur

vey images and making external bibliographic comparisons using the Strasb ourg VizieR

utility and SIMBAD

The tables are arranged as previously divided by region as in Homeisters lists A few

additional known variables that app ear in the nder charts are given for completeness

The Sonneb erg serial number and the GCVS designations app ear in the rst two columns

An asterisk by the GCVS name indicates a note which are collected at the end of the

tables The p ositions are taken mostly from USNOA Monet et al for some

brighter stars the GSC or ACT Urban et al was adopted and for a few crowded

00

stars p ositions have b een estimated  using largescale Digitized Sky Survey frames

from the Go ddard SkyView facility McGlynn et al The source of the p osition

is co ded in column s as follows A USNOA G GSC v S SkyView T

ACT

I made the matchup with the GSC using VizieR and found the various IDs in the

Remarks and Notes using SIMBAD The IDs are listed only if they are new in the sense

of b eing either not present or not linked in the same entry in SIMBAD

A few stars defeated my attempts to identify them Given that some of the stars I

did nd have p ositions several arcminutes in error it is likely that these lost ones have

similar errors of some kind The extremely crowded elds of Aquila and Sagitta made

matching the nder charts with the sky a challenging task

IBVS

Table North galactic p ole elds I

Sonne GCVS RA Dec s GSC Remarks

S AR Leo A

S AU Leo A

S CP Leo A

S AV Leo A

S AW Leo A

S BW Leo A

S CQ Leo A

S AZ Leo A

S BB Leo A

S BC Leo A

S BD Leo A

S BE Leo A

S BY Leo A

S BG Leo A

S BH Leo A

S BL Leo A

S CR Leo A

S CF Leo A

S BM Leo A

S BN Leo A

S CS Leo A

S CI Leo A

S CT Leo A

S CU Leo A



S CV Leo T BD

S BQ Leo A

S CK Leo A

S CL Leo A

S CM Leo A BPS BS

S VY Com A

S VZ Com A

S NSV A

S WW Com A

S WX Com A

S WY Com A

S XX Com A

S XY Com A BX Com S

S XZ Com A

S YY Com A

S CE Com A

S SN x A

S CH Com A

S ZZ Com A

S AA Com A

S FN Com A RXS J

S AE Com A BPS BS

S DD Com A

S AH Com A BPS BS

S DG Com A

S AN Com A

S AQ Com A

S AR Com A

IBVS

Table North galactic p ole elds I contd

Sonne GCVS RA Dec s GSC Remarks

S AT Com A

S AV Com A

S AY Com A

S BE Com A

S BF Com A BPS BS

S FR Com A

S BG Com A

S FG Com A

S BH Com A BPS BS



S NSV A BD

S FH Com A

S FI Com A

S BK Com A

S BM Com A

S BP Com A

S BR Com A

S BU Com A

S AF Bo o A

S AH Bo o A BPS BS

S AI Bo o A

S AL Bo o A

S AM Bo o A

S AN Bo o A

S BR Bo o A

S NSV A

S AQ Bo o A

S AT Bo o A

S AU Bo o A

S AV Bo o A

S AW Bo o A

S AX Bo o A

S AZ Bo o A

Table Aquilae eld

Sonne GCVS RA Dec s GSC Remarks

S NSV A

S V Aql A

S NSV A

S V Aql A

S V Aql A

S NSV A

S NSV A

S V Aql S

S V Aql A

S NSV A

S V Aql A

S V Aql A

S NSV S

S V Aql A IRAS

S V Aql A

S V Aql G IRAS

S V Aql A

IBVS

Table Aquilae eld contd

Sonne GCVS RA Dec s GSC Remarks

S V Aql A

S NSV A LF A

S V Aql S IRAS

S NSV A

S V Aql A

S V Aql not found

S V Aql A IRAS

S V Aql A

S NSV G

S V Aql A

S NSV A

S NSV A

S NSV A IRAS

S V Aql A IRAS

S V Aql G IRAS

S V Aql G IRAS

S V Aql A

S V Aql S IRAS

S NSV A

S NSV A IRAS

S V Aql A crowded

S V Aql A

S V Aql A IRAS



S NSV T BD

S V Aql A

S V Aql A

S V Aql A crowded

S NSV A IRAS

S V Aql A IRAS

S V Aql A

S V Aql A IRAS

S V Aql A IRAS

S V Aql A

S V Aql A

S V Aql A

S V Aql A

S V Aql A IRAS

S V Aql A

S V Aql A

S V Aql A IRAS

S NSV A

S V Aql A IRAS

S V Aql A IRAS

S V Aql A IRAS

S V Aql not found

S V Aql A IRAS

S V Aql A

S NSV A

V Aql A IRAS

S V Aql A

S V Aql A

IBVS

Table Aquilae eld contd

Sonne GCVS RA Dec s GSC Remarks

S V Aql A IRAS

S V Aql A

S V Aql A

V Aql G IRAS

S V Aql A

S V Aql A IRAS

S V Aql A

S V Aql A IRAS

S V Aql A IRAS

S V Aql A

S V Aql A

S V Aql A

S V Aql A

S V Aql A

S V Aql A IRAS

S V Aql A IRAS

S V Aql A IRAS

S V Aql A IRAS

S V Aql A

S V Aql A

S V Aql A

S V Aql A

S V Aql A IRAS

S V Aql A IRAS

S V Aql A

S V Aql S

S V Aql A

S V Aql A

S V Aql A

S V Aql A IRAS

S V Aql A IRAS

S V Aql A

S V Aql A IRAS

S V Aql A

S V Aql A IRAS

S NSV A

S V Aql A

S NSV A

S NSV A

S V Aql A

S V Aql A

S V Aql A southeastern of pair

S NSV A

S V Aql A IRAS

S V Aql A

S V Aql A

S V Aql A

S NSV A southern of pair

S V Aql not found

S NSV A

V Aql A IRAS

S V Aql S

IBVS

Table Aquilae eld contd

Sonne GCVS RA Dec s GSC Remarks

S NSV T

S NSV A IRAS

S V Aql A

S NSV G crowded

S V Aql A southern of two

S NSV S IRAS

S V Aql A crowded ID uncertain

S V Aql A southwestern of pair

S V Aql A

S V Aql A

S NSV A

S NSV A

S V Aql A

S V Aql A

S NSV A

S V Aql A IRAS

S V Aql A

S V Aql A

S V Aql A

S V Aql A

S V Aql A

S NSV A

S V Aql A

S V Aql A

S NSV A

S V Aql A

V Aql A IRAS

S V Aql A

S V Aql A

S NSV A

S V Aql A IRAS

S V Aql A IRAS

Table Aquilae eld

Sonne GCVS RA Dec s GSC Remarks

S V Aql A

S V Aql A

S V Aql A

S V Aql A

S NSV A IRAS

S NSV A

S NSV A IRAS

S NSV A IRAS

S V Aql A

S V Aql A double

S NSV A

S NSV A

S V Aql A

S V Aql A

IBVS

Table Aquilae eld contd

Sonne GCVS RA Dec s GSC Remarks

S V Aql A

S V Aql A

S NSV A

S V Aql A

S NSV A

S NSV A CGCS

S NSV A

S V Aql A

S NSV A PPM

S V Aql A

S V Aql A

S NSV A

S NSV A

S V Aql H

Table NGC eld I

Sonne GCVS RA Dec s GSC Remarks

S GV Cep A

S NSV A

S EN Cep A

S EQ Cep A

S ER Cep A

S ES Cep A

S ET Cep A

S NSV A

S EV Cep not found

S EW Cep not found

Table Delphini eld

Sonne GCVS RA Dec s GSC Remarks

S KR Del A IRAS

S KS Del A

S GH Del A

S KT Del A IRAS

S KU Del A

S KV Del A

S GI Del A

S FK Del A

S GK Del A

S GL Del A

S KX Del A IRAS

S HW Del A

S GM Del A

S GN Del A

S GO Del A

S GP Del A

IBVS

Table Delphini eld contd

Sonne GCVS RA Dec s GSC Remarks

S HY Del A

S GQ Del A

S GR Del A

S GS Del A

S GT Del A

S LM Del A

S GV Del A

S GX Del A

Table NGC eld

Sonne GCVS RA Dec s GSC Remarks

S NSV A

S NSV A

Table Sagittae eld

Sonne GCVS RA Dec s GSC Remarks

S V Aql A

S DN Sge A ID uncertain

S FX Vul A IRAS

S UU Sge A PN G

S MO Vul A

S DO Sge A

S GK Vul A IRAS

S GL Vul A

S DQ Sge A southwestern of pair

S V Aql A IRAS

S QW Sge G

S GS Vul A

S NSV A

S NSV A IRAS

S GT Vul A

S NSV T HD

S NSV A IRAS

S NSV A

S GW Vul C

S GZ Vul A

S NSV A

S NSV A IRAS

S HM Vul S

S HN Vul A

S NSV A

AS Sge S

S V Aql A

S DZ Sge A double

S NSV A

S NSV A

S EF Sge A

IBVS

Table Sagittae eld contd

Sonne GCVS RA Dec s GSC Remarks

S EE Sge S not NSV

S NSV A

S EG Sge A

S HO Vul A

S EK Sge A

S EN Sge A

S EO Sge A

S NSV A

S V Aql G

S NSV A

S HT Vul A

S NSV A

S EP Sge A

S EQ Sge A southern of close pair

S EX Vul A

S HV Vul A

S HU Vul A

S NSV A

S NSV A

S NSV A

S ET Sge A

S NSV A

S EV Sge A crowded

S V Aql S IRAS

S EW Sge A

S EY Sge A

S HZ Vul A

S FK Sge A

S FQ Sge A

S I I Vul A

S FR Sge A

S NSV A

S NSV A

Table  Cygni eld

Sonne GCVS RA Dec s GSC Remarks

S NSV A

S V Cyg A

S V Cyg A IRAS

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A IRAS

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A not IRAS

S V Cyg A

S V Cyg A

IBVS

Table  Cygni eld contd

Sonne GCVS RA Dec s GSC Remarks

S NSV A

S V Cyg A IRAS

S V Cyg A

S V Cyg A Cl NGC PLAT

S V Cyg A southern of pair

S V Cyg A Cl NGC PLAT

S V Cyg A

S V Cyg A

S V Cyg A IRAS

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S NSV A

S V Cyg A

S V Cyg A

S V Cyg A IRAS

S V Cyg A IRAS

S V Cyg A

S V Cyg A IRAS

S V Cyg A

S V Cyg A IRAS

S V Cyg A

S NSV A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S V Cyg A

S NSV A

S FU Lac A

S V Lac A

S V Lac A

S V Cyg A

Table  Puppis eld I

Sonne GCVS RA Dec s GSC Remarks

S HQ Pup G

S NSV A IRAS

S NSV A

S NSV A

S HX Pup A

S HY Pup A

S NSV A

S NSV G

S HZ Pup A Nova Pup

S I I Pup A IRAS

S FG Pup A

IBVS

Table  Puppis eld I contd

Sonne GCVS RA Dec s GSC Remarks

S IP Pup A

S NSV A

S IQ Pup A

S LZ Pup A

S IS Pup A

S NSV A

S NSV A

S IW Pup A

S NSV A IRAS

S NSV A IRAS

S NSV A IRAS

Table  Cassiop eiae eld

Sonne GCVS RA Dec s GSC Remarks

S V Cas A

S NSV A IRAS

S V Cas A

S V Cas A

S V Cas A IRAS

S V Cas A IRAS

S V Cas A IRAS

S V Cas A

S V Cas A IRAS

S V Cas A

S V Per A

S KU Per A

S V Cas A

Table NGC eld

Sonne GCVS RA Dec s GSC Remarks

S HL Gem A

S HM Gem A

S HN Gem A

S HO Gem A

S HP Gem A

S HQ Gem A

S HS Gem A

S HT Gem A

S NSV A

Table NGC eld I I

Sonne GCVS RA Dec s GSC Remarks

S EP Cep A

S EU Cep A

IBVS

h m 

Table PerseusAuriga

Sonne GCVS RA Dec s GSC Remarks

S NV Per A

S NW Per A IRAS

S OP Per A

S NSV A IRAS

S HV Aur A

S NSV A IRAS

Table North galactic p ole elds I I

Sonne GCVS RA Dec s GSC Remarks

S NSV A

S BF Leo A

S BZ Leo A

S BK Leo A

S BR Leo A

S NSV A

S BX Com A XY Com S

S CC Com G RXS J

S YZ Com A

S AB Com A

S DF Com A double

S DY Com A

S AS Com A

S AU Com A

S AZ Com A

S BI Com A

S BN Com A

S AK Bo o A

S BS Bo o A

S BV Bo o A

S A Cl NGC SAW V

S AO Bo o A

S BB Bo o A

S BE Bo o A

S BU Bo o A

Table  Puppis eld I I

Sonne GCVS RA Dec s GSC Remarks

S HT Pup A

S NSV A IRAS

S NSV A

S IL Pup G

S IO Pup A

S NSV A IRAS

S NSV A IRAS

S NSV A IRAS

S NSV A IRAS

S NSV A

S NSV A

S NSV G

S NSV G

S KK Pup A

S KL Pup A

S NSV A

S TW Pyx A

IBVS

Table AE Aurigae eld

Sonne GCVS RA Dec s GSC Remarks

S EW Aur A

S IK Aur A

S IL Aur A

S IO Aur A

S IP Aur A

S IR Aur A

S NSV A IRAS

S NSV A

S IT Aur A

S IV Aur A

S IW Aur A

Notes

V Aql faint on POSSI bright on POSSI I

s 00

V Aql ID uncertain alternate candidate at endgures :

V Aql crowded

V Aql GSC p osition oset in Dec from crowding

V Aql southwestern star of pair evidently not a dwarf nova but a Mira

cf Gessner

0

V Aql GCVS p osition in error

V Aql double Homeister suggests variable is the southeastern comp onent

V Aql NSV

V Aql GSCA p ositions slightly skewed by companion variable is

the eastern star of pair

V Aql IRAS p osition has large error ellipse

V Aql northeastern star of pair

IR Aur not double as p er Homeister

AF Bo o sup erp osed on the faint galaxy NGP F

V Cas Cl NGC LMM star marked is not red

BN Com ID uncertain northwestern star of pair

V Cyg northernbrighter star of pair

V Cyg also CGCS

KX Del star marked is red IRAS source

UU Sge SIMBAD p osition somewhat in error

ET Sge Downes et al p osition adopted

s 00

QW Sge southern star of pair companion at endgures : A

V BV FV cf Munari Buson

NSV also IRC

s 00

NSV ID uncertain is p ossibly fainter star at endgures :

NSV northeastern star of pair GSC p osition is for mean of pair

NSV coincident with IRAS but large error ellipse

SN x p osition is for host galaxy which is IRAS and Anon

References

Downes R A Webbink R F and Shara M M Publ Astron Soc Pac

Gessner H IBVS No

Gessner H Vero Sternwarte Sonneberg

Homeister C Astron Nachr

McGlynn T Scollick K and White N httpskviewgsfcnasagov see also

SkyView The MultiWavelength Sky on the Internet in McLean B J et al New

IBVS

Horizons from MultiWavelength Sky Surveys IAU Symp osium No p

Kluwer

Monet D Bird A Canzian B Harris H Reid N Rho des A Sell S Ables H

Dahn C Guetter H Henden A Leggett S Levison H Luginbuhl C Martini

J Monet A Pier J Riep e B Stone R Vrba F Walker R USNOA

US Naval Observatory Washington DC see also httpwwwusnonavymilpmm

Munari U and Buson L M Astron Astrophys

Ski B A IBVS No

Urban S E Corbin T E and Wyco G L Astron J

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

FASTT VERSUS IRAS

BRIAN A SKIFF

Lowell Observatory West Mars Hill Road Flagsta AZ USA email baslowelledu

In the course of work on the Wachmann SA variables Ski a and the Chavira

infrared stars Ski b I noticed numerous identications within SIMBAD involving a

list of susp ected variables found by Henden Stone using the USNOFlagsta

cm transit circle dubb ed FASTT Flagsta Astrometric Scanning Transit Telescope

Although ab out of the stars were accurately matched within the GCVS see

Henden Stones Table other external identications were not made

I have compared the list against the IRAS p ointsource and IRAS faintsource cat

alogues using the Strasb ourg VizieR facility The table shows the o dd matchups

00

found within of the highprecision FASTT co ordinates This search radius is similar

to the ma jor axis of the typical IRAS p osition errorellipse In fact the great ma jority

00

of the IRAS sources were within  of the FASTT star All but a few of these cor

resp ond to co ol AGB variables where the m IRAS ux ratios are  : with

generally no detection at m or m cf Figure of Zijlstra et al The only

two IRAS coincidences having o dd IRAS colors are two extragalactic ob jects one is a

quasar FASTT the other is the center of a nearby galaxy FASTT NGC

Since the FASTT astrometric reference frame included extragalactic radio sources

cf Stone highz ob jects were commonly on the observing program

The table preserves the precise  mas co ordinates of the online version of the orig

inal le I have made the p ositive Declination signs explicit however The next column

shows IRAS names While all the ordinary IRAS p ointsources are present in SIMBAD

most of the faintsource catalogue ob jects are not unless there is some published study

of them The last column shows various new IDs sp ecically names not linked with the

FASTT stars in SIMBAD If the IRAS name is already linked with a variablestar name

in SIMBAD then the GCVS name alone is given This is to emphasize the GCVS name

as a primary identier for the ob ject A few longer notes are given at the b ottom of the

list

I appreciate the comments of Arne Henden on the results of this search

IBVS

Table Identications for FASTT susp ected variables

FASTT RA Dec IRAS Identications

SX Cet

F

NSV

TI

BD Eri

F

Ohio A quasar

V Mon

CGCS C

GSC

CGCS C

MW Mon

LRS

AE CMi

F

AF CMi

NSV

see note

SY Leo

StM

NGC galaxy nucleus

WX Vir

F NSV

DW Ser

CL Ser

AI Ser

NSV

IBVS

Table Identications for FASTT susp ected variables contd

FASTT RA Dec IRAS Identications

CM Ser

V Oph

F

V Oph

V Oph

V Oph

V Oph

V Oph see note

F

V Oph

F

F

F V Oph

V Oph IRC

V Oph

F

AX Ser

F NSV

EQ Ser

YZ Ser

F

KT Oph

F

F

F V Oph see note

F

F

XY Ser

VZ Ser

V Oph

F

IBVS

Table Identications for FASTT susp ected variables contd

FASTT RA Dec IRAS Identications

V Oph IRC

V Oph

NSV

F

F

F

XZ Ser

IRC

IRC

IBVS

Table Identications for FASTT susp ected variables contd

FASTT RA Dec IRAS Identications

V Aql

VX Aql

Notes

CGCS C but not HIP whose co ordinates are for another star

ie Hipparcos missed the carb on star

evidently not IRAS outside p osition error ellipse

SIMBAD p osition in error cf Manek

References

Henden A A and Stone R C Astron J

data le httpvizierustrasbgfrvizbinCatJAJ

Manek J IBVS No

Ski B A a IBVS No

Ski B A b IBVS No

Stone R C Astron J

Zijlstra A Pottasch S and Bignell C Astron Astrophys Suppl Ser

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

COORDINATES AND IDENTIFICATIONS FOR

KUROCHKINS VARIABLES NEAR M

BRIAN A SKIFF

Lowell Observatory West Mars Hill Road Flagsta AZ USA email baslowelledu

The tables b elow show identications and accurate co ordinates for ab out variables

 

studied by Kuro chkin in a  region around the globular

cluster Messier Most of the variables were newly discovered Additional followup

work on the same stars was published much later Kuro chkin Although some of

the variables have precise p ositions published in more recent literature most do not

The format is identical to recent previous lists and broken into the four parts in which

they were published The rst column shows SVS numbers and the second the GCVS

designation An asterisk by the GCVS name indicates a note following the tables Nearly

all the p ositions come from USNOA but a few are from either the GSC v or

from largescale Digitized Sky Survey images from the Go ddard SkyView facility The

source is co ded in column s as follows A USNOA G GSC v S SkyView

Many ob jects were veried using DSS images and other sources All but one or two were

unambiguously identied from Kuro chkins charts

The present list was integrated into SIMBAD b efore publication by Fabienne Woelfel

CDSStrasb ourg She indep endently found the VV Cyg mixup which I had

missed Nikolai Samus Sternberg Institute Moscow provided the earlier Makarenko

citation for this correction I am grateful to them b oth for their interest in this work

IBVS

Table Positions and identications I

SVS GCVS RA Dec s GSC Remarks

V Lyr A

V Lyr A

V Lyr S

V Lyr A

V Lyr A

NSV A

NSV A

V Cyg A

V Lyr A

V Cyg A

V Cyg A

V Cyg A

V Cyg A

NSV A

V Cyg A

NSV A

NSV A

NSV A

V Cyg A

V Cyg A

Table Positions and identications I I

SVS GCVS RA Dec s GSC Remarks

NSV A

NSV A

V Lyr A

V Lyr A

V Lyr A

V Lyr A

V Lyr A

V Lyr A

V Lyr A

V Lyr A

V Lyr A

V Lyr A

NSV A

NSV A

NSV A

NSV A

MN Vul A

V Cyg A

V Cyg A

V Cyg A

HW Cyg G

IBVS

Table Positions and identications I I I

SVS GCVS RA Dec s GSC Remarks

V Lyr not found

V Lyr A

V Lyr A

V Lyr A IRAS

V Lyr A

V Lyr A

V Lyr A

V Lyr A

LY Vul A

V Lyr A IRAS

V Lyr A

V Lyr A

V Lyr A

V Lyr A

V Lyr A

AI Lyr A

V Lyr A

V Lyr A IRAS

OY Lyr A

V Lyr S

LZ Vul A

V Lyr A

V Lyr A

V Lyr A IRAS

V Lyr A

MM Vul A

V Lyr A

V Lyr A IRAS

V Cyg A

V Lyr A

Table Positions and identications IV

SVS GCVS RA Dec s GSC Remarks

NSV A

MP Vul A

MQ Vul A

V Lyr A IRAS

MR Vul A

V Cyg A

MS Vul S IRAS

V Cyg A

V Cyg S

MT Vul A IRAS

V Cyg A

V Cyg A

V Cyg A

EK Cyg A

V Cyg A

V Cyg A IRAS

V Cyg A

NSV A IRAS

IBVS

Notes

V Lyr Downes et al identication adopted

V Lyr veried on POSSI not visible on O blue print

d

MT Vul red variable with P  not an eclipser as rst susp ected

cf Kuro chkin

V Cyg given erroneously as V Cyg by Kuro chkin corrected

by Makarenko

V Cyg southern star of a pair

References

Downes R A Webbink R F and Shara M M Publ Astron Soc Pac

Kuro chkin N E Perem Zvezdy

Kuro chkin N E Perem Zvezdy

Kuro chkin N E Perem Zvezdy

Kuro chkin N E Perem Zvezdy

Kuro chkin N E Perem Zvezdy

Makarenko E N Perem Zvezdy Prilozh

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

PHOTOELECTRIC BVI OBSERVATIONS AND NEW ELEMENTS

C

FOR THE CEPHEID V CENTAURI

1;2 3;4 5

L N BERDNIKOV V V IGNATOVA D G TURNER

1

Sternberg Astronomical Institute Universitetskij prosp Moscow Russia

2

South African Astronomical Observatory

3

Tashkent University Department of Astronomy

4

Astronomical Institute Astronomicheskaya st Tashkent Uzb ekistan

5

Saint Marys University Halifax Nova Scotia BH C Canada

Name of the ob ject

V Cen GSC HIP

Equatorial co ordinates Equinox

h m s  0 00

RA DEC

Observatory and telescop e

South African Astronomical Observatory m reector

Detector Photomultiplier Hamamatsu

Filters BVI

c

Comparison stars No We conducted all sky photometry

Check stars No See ab ove

Transformed to a standard system BVI

c

Standard stars eld used Standard stars from Eregions

Availability of the data

Through IBVS Website as ttxt

Type of variability DCEPS

Table

Max JD hel Number of

Uncertainty E O C Reference

observations

 HIPPARCOS data

 HIPPARCOS data

 HIPPARCOS data

 This pap er

IBVS

V V898 Cen P=3.527 7.8 8.1 B-V 0.6 0.8 V-I C 0.7 0.9

0.0 0.5 1.0 Phase

Figure

Remarks

Variability of V Cen was announced by Strohmeier et al According to

HIPPARCOS data this star HIP is a Cepheid variable with elements

d

Max JD  E

hel

m

The accuracy of our individual data is near in all lters We analysed all

existing observations by Hertzsprungs metho d Berdnikov and the derived

ep o chs of light maximum are given in Table The times of light maximum were in

tro duced into a linear leastsquares program that resulted in the following improved

ephemeris

d

Max JD  E

hel

 

This ephemeris was used to calculate the O C values in Table as well as for

plotting the light and colour curves in Figure

Acknowledgements

The research describ ed here was supp orted in part by the Russian Foundation

of Basic Research and the State Science and Technology Program Astronomy

to LNB and through NSERC Canada to DGT We would also like to express our

gratitude to the administrations of SAAO for allo cating a large amount of observing

time

References

Berdnikov LN Sov Astron Lett

Strohmeier W Knigge R Ott H IBVS No

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

PHOTOELECTRIC VI OBSERVATIONS AND NEW CLASSIFICATION

C

FOR RV NORMAE

1 2

L N BERDNIKOV D G TURNER

1

Sternberg Astronomical Institute Universitetskij prosp Moscow Russia

email b erdniksaimsusu

2

Saint Marys University Halifax Nova Scotia BH C Canada

Name of the ob ject

RV Nor GSC

Equatorial co ordinates Equinox

h m s  0 00

RA DEC

Observatory and telescop e

South African Astronomical Observatory m reector

Detector Photomultiplier Hamamatsu

Filters VI

c

Comparison stars No We conducted the all sky photometry

Check stars No See ab ove

Transformed to a standard system VI

c

Standard stars eld used Standard stars from Eregions

Availability of the data

Through IBVS Website as ttxt

Type of variability RV

Remarks

RV Nor is listed in the GCVSIV as a type I I Cepheid with the elements

d

Max JD  E

that are used in Figure for plotting our data The accuracy of the individual

m

observations is near in all lters It is obvious that these elements are not

valid and if RV Nor is p erio dic variable it is most probably an RVTAU type

star with a p erio d near twice of ab ove one Using Harris observations we

obtained the following ephemeris

d

Min JD  E

This ephemeris is used in Figure

IBVS

Acknowledgements

The research describ ed here was supp orted in part by the Russian Foundation

of Basic Research and the State Science and Technology Program Astronomy

to LNB and through NSERC Canada to DGT We would also like to express our

gratitude to the administrations of SAAO for allo cating a large amount of observing time

V RV Nor P=32.33 12.1

13.8 V-I C 1.5 1.9

0.0 0.5 1.0 Phase

Figure Small circles and dots represent our Figure Observations obtained b efore and af

observations large circles represent data from ter JD identied by circles and dots re

Harris whose intermediateband measure sp ectively

ments were converted to V I using formulae

c

from Coulson et al

References

Coulson IM Caldwell JAR Gieren WP Astrophys J Suppl Ser

Harris H PhD Thesis University of Washington

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

NSV A LYRAE TYPE ECLIPSING BINARY

J VANDENBROERE

Group e EuropeendObservations Stellaires GEOS Promenade Venezia F Versailles

Email jvandenbroereskynetb e

NSV  GSC  HV  P is catalogued as a p ossible

eclipsing or irregular variable from a list published by Shapley and Hughes and

from irregular variations detected by Sandig on photographic plates The Lyrae

shap e of its light curve was obvious from the visual estimates of several GEOS members

and its orbital p erio d app eared to b e days Vandenbroere

Figure V and B V Geneva system light curves of NSV

This value was used to collect new and more accurate photo electric data Therefore

h m s  0

NSV was measured with the cm telescop e of the

Jungfraujo ch station through the B and V lters of the Geneva system measurements

were obtained in each lter b etween January and December The folded V and

IBVS

Figure Dierent b ehaviours were observed in the phase interval

m

B V light curves are shown in Fig NSV is a Lyrae star with V

m

at maximum light a primary minimum as faint as V and a secondary one going

m

down to V The B V colour indices vary slightly from to

G

which corresp onds to a B V index of to after transformation with the

J

formulae describ ed by Meylan and Hauck and using the luminosity class I I I

A more accurate orbital p erio d was calculated by means of the primary and secondary

photo electric minima and of instants extracted from the visual estimates of three GEOS

members The result of the linear regression giving a triple weight to the photo electric

moments is

d

Min I HJD  E

 

A close insp ection of Fig shows irregularities in the shap e of the light curve par

ticularly on the shoulders b efore b oth maxima Note also the related b ehaviour of the

B V curve which mimics the V one Probably the star is undergoing mass exchanges

and shorttime scale variability is resp onsible for the scatter around the phase

interval as b etter evidenced in Fig

The author wishes to thank N Beltraminelli R Boninsegna G DineZepter and

J Remis for helping in obtaining the photo electric data D Dalmazio and A Manna for

their visual estimates

References

Meylan G and Hauck B AAS

Sandig HU Astron Nachr

Shapley H and Hughes EM Harvard Annals

Vandenbroere J Note Circulaire GEOS NC

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

V V AND FOUR NEW VARIABLE STARS IN THE FIELD OF M

T RUSSEVA

Institute of Astronomy Bulgarian Academy of Sciences Tzarigradsko shosse bld BG Soa Bulgaria

email russevatastrobasbg

M NGC is a galactic globular cluster lying on a rich stellar eld at

h m  0  

l b

The Third Catalogue of Variable Stars in Globular Cluster SawyerHogg con

tains three red variable stars V V and V in M with unknown p erio ds These stars

are physical members of the cluster according to their prop er motions Rishel et al

and the p osition in the colourmagnitude diagram Barb on and Russev

We have investigated the variability of these three variables as well as red giants The

latter fall on the red giant branch RGB in the colourmagnitude diagram of M at

m

B V

This study is based on blue plates ZU emulsion GG lter and plates

in system V aD emulsion GG lter taken with the m telescop e of the NAO

Rozhen Bulgaria and with the cm reector of the Belogradchic Astronomical sta

tion Bulgaria during years from to All plates were measured with an

iris diaphragm photometer using Barb ons standard sequence and a photo electric

sequence kindly placed at our disp osal by Russev unpubl The photometric error is

 mag

New Variables As a variability criterion of the investigated program stars we have

!

B B

i

B obtained from of their mean magnitudes adopted the mean error

n

the available individual measurements B It was assumed that we could susp ect in

i

variability those stars which have larger than the accuracy of the photometry Table

lists the stars susp ected in variability The columns and give K ustner

Barb on and Rosino numbers of the stars resp ectively The next columns

B the number of their measurements give the average values of the blue magnitudes

the mean error and the average values of colours B V

Stellingwerf s PDM metho d was used for searching the p erio ds of the program

stars We have not found any evidence for variability of the stars with Nos

and in K ustners catalogue The analysis has shown that K

K K and K are undoubtedly variable stars The light curve elements are

d

Max JDH  E for K

d

Max JDH  E for K

d

Max JDH  E for K

d

Max JDH  E for K

IBVS

Table A list of the investigated red giants and red variable stars in M

K No B No R No B n B V lg P A 4f

B

I

I

I

I

V

V

V

and their phase curves are shown in Fig From the average light curves we obtained

the amplitudes A and asymmetry parameters 4f f f of the stars Table

B min max

columns and

The question of the membership of the investigated ten red giants is very imp ortant

The stars K and K are cluster members according to their prop er motions Rishel

et al and K and K according to the radial velocity measurements Harris

et al The rest stars including the three new variables probably b elong to the

cluster by their p ositions in the colourmagnitude diagram and their distances from the

00 00 00

cluster center for K K and K It should b e noted

however that any solution of the problem of the cluster membership for the new variable

stars has to await from the results of the other two criteria such as prop er motion and

radial velocity measurements

V V and V The light curves of V and V constructed with help of the following

elements

d

Max JDH  E for V

d

Max JDH  E for V

and their phase curves are shown in Fig Two p erio ds seem to t the observations of

d

V The alternative p erio d pro duced a b etter light curve for Wehlau and Sawyer

Hoggs data from OHP and UWO plates We consider the light curve of V as

preliminary and requiring sp ecication The scattering in the light curves Fig and

is probably due to sudden changes in brightness or shifting of the light curve maxima

similar to those observed for L and L in M by Russev and Russeva and

Russeva and Russev

The analysis of the data for V has not indicated any variability

m m

V for V and for V The variables V and V are the brightest

m m

and the reddest B V and for V and V resp ectively stars in M

According to their p erio ds amplitudes and shap e of the light curves the variables V V

and K fall in the group of the smaller amplitude variables in the globular clusters with

d d

p erio ds from to As it is known such stars are found comparatively rarely among

the variables of this type in such aggregates The comparison with the red variable stars

in M and in other globular clusters in our Galaxy is necessary

IBVS

Figure Light curves of new red variables in the eld of M The size of the symbols is prop ortional

to the number of observations p er night

Figure Light curves of V and V The size of the symbols is the same as in Fig

IBVS

References

Barb on R Asiago Obs Contrib No

Harris H Nemec M and Hesser E PASP

K ustner F VeroU Sternw Bonn No

Rishel B Sanders W and SchoderR AA Suppl

Rosino L Asiago Obs Contrib ser VI I I v X

Russev RM in the press

Russev RM and Russeva T IBVS No

Russeva T and Russev RM IBVS No

Sawyer Hogg H Publ David Dunlap Obs No

Stellingwerf RF ApJ

Wehlau A and Sawyer Hogg H AJ

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

GSC A SUSPECTED NEW VARIABLE

PRISCILLA J BENSON AND DEMERESE M SALTER

Whitin Observatory Wellesley College Wellesley MA

email pb ensonwellesleyedu dsalterwellesleyedu

Name of the ob ject

GSC

Equatorial co ordinates Equinox

h m s  0 00

RA DEC

Observatory and telescop e

Sawyer telescop e at Whitin Observatory Wellesley College

Detector Photometrics PM CCD for observations from

June through June and Photometrics TK AB

CCD Camera b eginning July

Filters Johnson and Cousins B V RI

Comparison stars GSC

Check stars GSC

Transformed to a standard system Yes

Standard stars eld used Transformations of dierential

data use M as standards Trans

formation of Mt Hopkins data

used Fields SA stars

and SA stars

of Landolt

Type of variability Possibly Small Amplitude Red Variable

IBVS

Remarks

The variability was discovered while monitoring the activity of symbiotic star BF

Cygni using dierential photometry at Whitin Observatory It was noticed during

the analysis that one of the comparison stars for BF Cygni was showing a larger

variation in brightness than the other comparison stars The magnitudes of the

comparison stars in the eld were obtained using the Smithsonian telescop e

with a standard B V RI lter set at Whipple Observatory on Mt Hopkins

September All sky photometr y was done using Landolt standard stars

in the SA and SA elds The eld is shown in Figure with BF Cygni

the susp ected new variable the comparison star and the check star all identied

The magnitudes of the four identied stars fr om the Whipple Observatory data

are given in Table We note that the susp ected variable had a B V color of

on that date

From the dierential photometry taken at Wellesley College we nd the susp ected

m m m m

new variable varies from ab out to in V amplitude to

m m m m m

in R amplitude and to in I amplitude The

standard deviation of the dierential magnitude b etween the susp ected variable

and the comparison star is ab out three times larger than that for the dierential

magnitude b etween the comparison and check stars as can b e seen in the light

curves in Figure No evidence of p erio dicity was found

Table

Star RA Dec B mag V mag R mag I mag

h m s  0 00

BF Cygni

h m s  0 00

NSV GSC

h m s  0 00

Comp GSC

h m s  0 00

Check GSC

Acknowledgements

This research made use of the SIMBAD database op erated by the CDS Stras

b ourg France and the NASA Astronomical Data Center We thank the Fairchild

Foundation Grant to Wellesley College for a summer internship DMS and W

M Keck Foundation for supp ort o f astronomy at Wellesley College through the

Keck Northeast Astronomy Consortium This research was also partially supp orted

by funds from the National Science Foundation AST and the Wellesley

College Brachman Homan Fellowship PJB

References

Landolt A U Astron J

Landolt A U Astron J

Landolt A U Astron J

IBVS

Figure The nder chart for the new variable North is up and East is left The size of the eld shown is ab out arcminutes square

New Variable in BF Cygni Field in V Filter

.6

.8

1

Differential Magnitude 1.2 49400 49600 49800 50000 50200 50400 50600 50800 51000 51200 Julian Day - 2400000

New Variable in BF Cygni Field in R Filter

-.1

0

.1

.2

.3

Differential Magnitude .4 49400 49600 49800 50000 50200 50400 50600 50800 51000 51200

New Variable in BF Cygni Field in I Filter

-.9

-.8

-.7

-.6

-.5

Differential Magnitude -.4

49400 49600 49800 50000 50200 50400 50600 50800 51000 51200

Figure Light curves for the new variable lled circles Op en circles denote the magnitude dierence b etween the comparison and the check star

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

STROMGREN PHOTOMETRY OF THE Be STAR  CrB

SAUL J ADELMAN

Department of Physics The Citadel Moultrie Street Charleston SC USA

email adelmanscitadel edu

Fabregat Adelman presented dierential Stromgren uv by photometry from

the Four College Automated Photo electric Telescope FCAPT of the Be star Coronae

Borealis HR HD obtained during February and March and

during March through July No short term p erio dic variability with an amplitude

m m

greater than nor long term variations greater than were seen A review of

the literature shows that CrB has had p erio ds of b oth activity and inactivity see eg

Percy et al and Percy Attard Thus the photometric observations with the

FCAPT were continued to see how long the p erio d of inactivity would last

The FCAPT op erated on Mt Hopkins AZ for six years until July and since then

at nearby Washington Camp AZ During the and

observing seasons an additional and high quality observations resp ectively

were made with the FCAPT Table summarizes the photometry the values are not

identical with those of Fabregat Adelman as a few values were deleted After

the dark count the telescop e measures the sky ch c v c v c v c ch sky in each

lter with sky b eing a reading of the sky ch of the check star c of the comparison star

and v of the variable star Table contains group a variable along with two supp osedly

nonvariable stars the comparison and check against which the brightness of the variable

is compared information Hoeit ESA The comparison and check stars were

chosen from supp osedly nonvariable stars in the vicinity of the variable on the sky that

had similar V magnitudes and B V colors Their stability was checked using Hipparcos

photometry ESA by Adelman The Hipparcos photometry standard errors

and amplitudes of CrB are the same as those of the comparison and check stars which

are considered to b e nonvariable It is usually dicult to nd stars of a given type with

smaller standard errors and amplitudes esp ecially close to a given p osition in the sky

The consensus of the users of the FCAPT is that its dierential photometry has an

m

accuracy of order for prop erly exp osed stars Thus apparent systematic dierences

of this magnitude must b e regarded with caution Further one must b e careful of any

changes o ccurring at the time the telescop e was moved as they might b e due to small

errors in the extinction such as those in u The y photometry of CrB is the most stable

m

The largest changes were in b where the v c values brightened by ab out b etween

and but this might b e due to the comparison star

The study of Be stars which are not always variable should b e able to yield imp ortant

information ab out this class The formation and disp ersion of the equatorial disk is the

IBVS

Table Summary of photometry for CrB

Helio centric u v b y

Julian Date v c c ch v c c ch v c c ch v c c ch

observations

average

std dev

observations

average

std dev

observations

average

std dev

observations

average

std dev

observations

average

std dev

observations

average

std dev

all observations

average

std dev

Table Main data for the stars involved

Sp ectral Hipparcos

Star V Type std error amplitude

Var HD CrB BVnne

Comp HD Bo o BVn

Check HD Bo o AV

IBVS

source of the variability on various time scales By obtaining long term photometric

data one can derive information on the nature of the variability and its relationship to

variability at other wavelengths Since observations of how a variability episo de b egins in

CrB should b e most enlightening this series of observations will b e continued As this

star has b een inactive since ab out Percy Attard it might b ecome variable

in the next few years But the FCAPT photometry has not yielded any information ab out

changes in its current nonvariable state as the standard deviations of the means so far

have reected mainly the observing conditions under which the data was taken

Acknowledgments This work was supp orted in part by NSF grants AST and

and in part by grants from The Citadel Development Foundation I appreciate

the continuing eorts of Louis J Boyd Rob ert J Dukes Jr and George P McCo ok to

keep the FCAPT op erating prop erly

References

Adelman S J Baltic Astronomy

ESA The Hipparcos and Tycho Catalogues ESA SP

Fabregat J Adelman S J AA

Hoeit D The Bright Star Catalogue th edition Yale University Observatory

New Haven CT

Percy J R Con B L Drukier G A et al PASP

Percy J R Attard A PASP

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

June

HU ISSN

GSC IS A NEW VARIABLE STAR

YURIJ N KRUGLY

Kharkiv Observatory Sumska str Kharkiv Ukraine kruglyastronkharkovua

Name of the ob ject

GSC

Equatorial co ordinates Equinox

h m s  0 00

RA DEC J

Observatory and telescop e

Astronomical Observatory of Kharkiv State University cm telescop e

Detector STV CCD

Filters V

Transformed to a standard system V close to the standard Johnsons

system

Standard stars eld used Field P from Lasker et al

Availability of the data

Through IBVS Website as ttxt

Type of variability SXPHE

Remarks

Discovered as a byproduct of CCD observations of the asteroid RaShalom

Image reductions and photometry AstPhot package Mottola et al The

m m

star shows rapid Delta Scutilike variations b etween and V Prelimi

nary light elements from two maxima the rst of them incompletely covered

d

Max hel  E



The star is at a high galactic latitude b so the star probably b elongs to

the SX Phe subtype of Delta Scuti variables

References

Lasker BM Sturch CR Lop ez C et al Astrophys J Suppl Ser

Mottola M De Angelis G Di Martino M et al Icarus

IBVS Figure

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

July

HU ISSN

HIPPARCOS PARALLAXES OF CATACLYSMIC BINARIES

y

AND THE QUEST FOR THEIR ABSOLUTE MAGNITUDES

HILMAR W DUERBECK

University of Brussels VUB Pleinlaan B Brussels Belgium email hduerb ecvubacb e

Hipparcos prop osal No submitted in by N Vogt Th SchmidtKaler and

the present author suggested several novae novalike stars and dwarf novae for measure

ments of parallaxes and prop er motions Unfortunately SS Cyg the only dwarf nova of

the prop osal was not observed due to a misidentication A comparison b etween the Cat

alogue of Cataclysmic Variables Downes Shara and Webbink and the Hipparcos

catalogue pro duced no additional cataclysmic variables identied after completion of the

Hipparcos Input Catalogue that might have b een included by chance in the target list

Table Parallaxes and distances of Hipparcos novae and novalike systems

00 00

HIP Ob ject parallax distance d  error p c

Novae

RR Pic

T CrB

V Aql

HR Del

Novalike systems

IX Vel

RW Sex

QU Car

V Sgr

AE Aqr

Table lists the parallaxes in milliarcseconds of the nine cataclysmic variables as

given in the Hipparcos catalogue ESA and their derived distances It should b e

noted that the ob jects were selected b ecause of apparent brightness not b ecause of the

p otentially large parallax Most cataclysmic variables at minimum light even p otentially

near ones are b elow the magnitude limit of the Hipparcos satellite The following

discussion confronts the Hipparcos results with other presentday information

Novae RR Pic The Yale parallax catalog van Altena Lee and Hoeit gives

abs  N with the quality mark go o d agreement This is

within the errors of the Hipparcos result

y Based on data from the ESA HIPPARCOS astrometry satellite

IBVS

V Aql The Yale parallax catalog gives abs  N with

the quality mark go o d agreement This is in excellent agreement with the Hipparcos

result

Berriman Szkody and Capps give a distance of p c Novalike systems IX Vel

while Eggen and Niemela derive p c Beuermann and Thomas carried

out a careful analysis of this brightest UX UMa type system and derived the distance

d  p c from Baileys metho d This value is in excellent agreement with the

Hipparcos result

The Yale parallax catalog gives abs  N with RW Sex

the quality mark go o d agreement Beuermann Stasiewski and Schwope use

Baileys metho d which results in a rough estimate d  p c consistent with Osvalds

trigonometric parallax  as quoted by Cowley Crampton and Hesser

The Hipparcos parallax is consistent with these statements in spite of the large

error we assume that the true parallax is not much smaller than the value mas

QU Car Gilliland and Phillips derive d p c They state that the sp ectrum

is dominated by light from the accretion disk or the primary and that the high rate of

mass transfer indicates an old nova or novalike variable The sp ectroscopic app earance

He i i emission as strong as N i i iC i i i supp orts this The Hipparcos parallax is

in agreement with the ab ove distance estimate without b eing able to improve it

A sp ectroscopic analysis by Haug and Drechsel shows anticyclic He i V Sgr

absorption which cannot b e attributed to the secondary star They assume an inclination

 

i which is likely to o large Warner gives i and derives M from

V

the surface brightness metho d with m and A this results in the distance

V V

d p c The Hipparcos parallax indicates that this distance is overestimated An



inclination i would make the discrepancy even worse

The Yale parallax catalog gives abs  N ie AE Aqr

d p c which app ears to b e to o small The b est distance estimate is that

of Welsh Horne and Oke The sp ectral type of the secondary is most likely KK

V It contributes b etween and to the light at nm Using the BarnesEvans

relation and the equivalent Ro che lob e radius of the secondary Welsh et al estimate the

distance d  p c if the disk is hot and  p c if the disk is co ol The Hipparcos

distance lies comfortably in this range without b eing of use in deciding b etween the two

cases An extensive discussion of the parallax of this system and the question whether

the secondary is a main sequence star was given by Friedjung

Most trigonometric parallaxes of novae are small or vanishing the p ositive result of

V Aql is in agreement with the nebular expansion parallax d p c Duerb eck

The absolute magnitudes M of four novalike stars were derived from the Hipparcos

V

parallaxes Apparent magnitudes V were taken from the list of Bruch and Engel

interstellar extinction A was estimated using the programme of Hakkila et al

V

Absolute magnitudes of three dwarf novae at maximum were calculated from the Hubble

Space Telecope ne guidance sensor parallaxes of Harrison et al and absolute

magnitudes of novae in the interval of orbital p erio ds of the dwarf novae and novalike

systems considered here were derived from nebular expansion parallaxes Duerb eck

Information on inclinations i and orbital p erio ds P is taken from Ritter and Kolb

All absolute magnitudes M were corrected for inclination eects using the prescription

V

corr

of Warner and listed as M in Table In the case of unknown inclination i

V



was assumed to b e

IBVS

Table Absolute magnitudes of cataclysmic variables as derived from trigonometric and nebular ex

pansion parallaxes

 corr

Ob ject p erio d days V d p c A M i M

V V

V

Dwarf novae at outburst

SS Aur

SS Cyg

U Gem

Novalike systems

AE Aqr

V Sgr

RW Sex

IX Vel

Novae at p ostoutburst minimum

V Aql

T Aur

V Cyg

HR Del

DQ Her

V Her

BT Mon

RR Pic

1.0 BT

2.0

RR 3.0

4.0 RW M_V

5.0

6.0 AE

7.0 −1.0 −0.8 −0.6 −0.4 −0.2

log P [days]

Figure Absolute V magnitudes as a function of orbital p erio d in days Op en circles p ostnovae

from expansion parallaxes lled circles dwarf novae at outburst from HST parallaxes circles with

central dot novalike stars from Hipparcos parallaxes A few systems are identied the absolute

m corr

magnitude of RW Sex is uncertain by more than  The regression line M log P is

V shown

IBVS

The results are shown in Fig There is no obvious dierence b etween the absolute

magnitudes of dwarf novae in outburst novalike stars and novae a few decades after

outburst If the p oint in the lower right the p eculiar system AE Aqr which has no fully

developed accretion disk is not taken into account the remaining p oints indicate that

systems with longer p erio ds have brighter accretion disks The data however are to o

scarce to draw denitive conclusions We have omitted from our discussion outlying

novae of very short as well as very long p erio d CP Pup and GK Per which have absolute

corr

magnitudes M and resp ectively would mask this p ossible p erio d dep endence

V

The conclusion is In the interval day an absolute magnitude orbital p erio d

corr

relation M log P seems to exist for all types of cataclysmic systems novae

V

at minimum novalike systems dwarf novae at outburst where angularmomentumloss

controlled mass loss from the main sequence star feeds an accretion disk

Acknowledgement Most of this study was carried out while I was a visiting scientist at

the Space Telescope Science Institute Baltimore Thanks go to Nino Panagia and Mike

Shara for arranging my stay and to Ron Downes for providing an up dated version of the

Catalog of Cataclysmic Variables

References

Altena WF van Truenliang Lee J Hoeit D The General Catalogue of

Trigonometric Stellar Parallaxes Fourth ed Yale University Observatory New

Haven CT

Berriman G Szkody P Capps RW MNRAS

Beuermann K Thomas HC AA

Beuermann K Stasiewski U Schwope AD AA

Bruch A Engel A AAS

Cowley AP Crampton D Hesser JE PASP

Downes R Shara M Webbink R PASP

Duerb eck HW ApSS

Duerb eck HW unpublished compilation

Eggen OJ Niemela VS AJ

ESA The Hipparcos and Tycho Catalogues ESA SP

Friedjung M New Astr

Gilliland RL Phillips MM ApJ

Hakkila J Myers JM Stidham BJ Hartmann DH AJ

Harrison TE McNamara BJ Szkody P McArthur BE Benedict GF Klemola

AR Gilliland RL ApJ L

Haug K Drechsel H AA

Ritter H Kolb U AAS

Warner B MNRAS

Welsh WH Horne K Oke JE ApJ

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

July

HU ISSN

PHOTOMETRIC OBSERVATIONS OS NSV

1 1 2

P MERCHANBENTEZ M JURADOVARGAS F SANCHEZBAJO

1

Departamento de FsicaFacultad de Ciencias Universidad de Extremadura Ctra de Elvas Bada joz

Spain email p edromerunexes mjvunexes

2

Departamento de Electronicae IngenieraElectromecanicaEscuela de IngenierasIndustriales Universidad

de Extremadura Ctra de Elvas Bada joz Spain email fsanba jounexes

Name of the ob ject

NSV CSV

Equatorial co ordinates Equinox

h m s  0 00

RA DEC

Observatory and telescop e

Observatorio del Departamento de Fsica de la Universidad de Extremadura Re

ector Newton m f

Detector Starlight Xpress CCD Camera based in the chip SONY

ICXBL  mm  pixels

Filters V KronCousins system

Comparison stars GSC

Check stars GSC

Transformed to a standard system No

Availability of the data

Up on request

Type of variability RR Lyr

Remarks

The results of the observations carried out show that NSV seems to b e an

RR Lyrae star with a p erio d close to hours Although the data display a high

disp ersion the star shows an almost symmetric light curve and a

magnitude amplitude in the V band We have derived the following ephemeris for

the maximum

d

Max HJD  E

 

IBVS

Acknowledgements

This research was supp orted by the Consejerade Educaciony Juventud Junta de

Extremadura and Fondo So cial Europ eo under pro ject IPRA 15h40m 15h39m30s 15h39m

S 12 S 12

C

S 12 05’ S 12 05’

V

Ck S 12 10’ S 12 10’

15h40m 15h39m30s 15h39m

Figure Identication chart of NSV C comparison star Ck Check star V NSV

North is on the top

Figure The V light curve obtained for NSV Delta magnitudes variable minus comparison

are plotted versus phase where the phases are computed using the ephemeris calculated in this work

Reference

Kukarkin et al New Catalogue of Susp ected Variable Stars Moscow

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

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July

HU ISSN

A PHOTOMETRIC UPDATE ON  CORONAE BOREALIS

JD FERNIE

David Dunlap Observatory University of Toronto Canada email fernieastroutorontoca

CrB HR HD is a G giant star that has the unexp ected prop erty of

b eing chromospherically active Maggio et al found it to b e one of only two single

giants out of giants and sup ergiants studied that have an Xray ux as high as RS

Canum Venaticorum stars while Young Ajir and Thurman rep ort it to have one

of the highest Ca I I H and K reversal uxes among the many stars they surveyed Evans

found it to show ultraviolet emission lines such as C IV that were similar

to though less strong than those in And a chromospherically active G I I I star

Some years ago I accidentally discovered CrB to b e variable in light with a V ampli

tude of ab out mag and a quasip erio d near days Fernie

Since the fundamental radial pulsation p erio d of such a star would b e much less than

day and since the star is chromospherically active these results were interpreted in terms

of a starsp ot mo del in which a few large sp ots on a limited region of the stellar surface

mo dulate the light as the star rotates The photometric data were in the UBV system

and the fact that the amplitude was at least to rst order the same in each lter lent

supp ort to this interpretation The uctuating p erio d was interpreted as due to starsp ots

forming in andor drifting to dierent stellar latitudes which presumably have dierent

rotation rates Choi et al found similar photometric results and provide Ca II

ux measures which vary strongly and inversely with visual brightness as well as an ex

tended discussion on the nature of the star It might also b e noted that ONeal and Ne

in a study of other active stars used CrB as one of their inactive comparison

stars

CrB has remained on my Automatic Photometric Telescope program and I rep ort

here briey on the stars photometric b ehaviour since my last published data nearly a

decade ago The complete le of individual UBV observations is available from the

IAU Commission archives of unpublished data as le no E

The data were analysed by annual season this b eing a compromise b etween using

enough data to get meaningful results since the variability is small in the presence of

relatively noisy data on the one hand while minimizing the eects of the known p erio d

instability on the other Light curves for the seasons of higher amplitude are shown in

the ab ove cited pap ers

All the data for a given season were plotted against Julian Date and where a light

curve was discernible a simple rstorder sine curve was tted The amplitude mean

V magnitude p erio d and time of maximum light as determined by this t were then

recorded In the and seasons however no light curve was

IBVS

Figure The changing V amplitude of CrB with time The op en symbols represent upp er limits

Standard errors of the lled circles are approximately the size of the circles

Figure The change in mean magnitude with amplitude The op en symbols represent upp er limits on the detectible amplitude

IBVS

Table Amplitude mean mag

Year Ampl hV i

seen ab ove the noise and only the arithmetically averaged V magnitude was recorded

and an upp er limit on the amplitude estimated

For a sp otted star only a characteristic p erio d of variability can b e given b ecause of the

dierential rotation and the probably everchanging sp ot pattern near the stellar surface

This problem is aggravated by the small amplitude and long timescale of the variation

observed in the case of CrB For this giant star summing up the photometric and

sp ectroscopic observations obtained so far we may adopt a characteristic p erio d of the

light variations and hence the rotation as days

Figure illustrates the change in amplitude over the seasons It steadily declined

during the rst seasons since when it has remained at a barely detectable or unde

tectable level Thus if CrB has a sp ot cycle analogous to that of the sun these data

suggest it is longer than years It is also notable that whereas the solar cycle having

reached minimum immediately starts up towards maximum again in CrB it app ears to

remain at minimum for many years There may of course b e structure in Fig during

the later years that is hidden by the noisy data but if the cycle is sinusoidal then a dis

cernible rise should have b ecome apparent well b efore This extended interval near

minimum was probably a factor which contributed to this th magnitude star not having

b een found earlier to b e variable

Figure addresses the question of whether the overall brightness of the star varies with

amplitude that is with degree of activity The mean magnitude in this plot is derived

from a sinusoidal t to the light curve or in seasons of no discernible light curve from

an average of all the seasons V measurements The internal standard error of each p oint

is ab out the size of the symbol in the gure so there do es seem to b e a slight but denite

change in brightness with amplitude although the functional relationship is unclear and

likely involves other parameters as well At minimum amplitude the star is very close to

V and as activity b egins there is an initial fading towards V p ossibly

caused by the increasing area of dark sp ots When most active however the star is

brighter than usual p erhaps b ecause bright plages overwhelm the dimming eect of the sp ots

IBVS

It is a pleasure to thank the APT managers for their inestimable services I am also

grateful to Dr Katalin Olahfor her suggestions as referee

References

Choi HJ So on W Donahue RA Baliunas SL and Henry GW PASP

Evans NR Private Communication

Fernie JD PASP

Fernie JD PASP

Fernie JD PASP

Fernie JD PASP

Maggio A Vaiana GS Haisch BM Stern RA Bo okbinder J Harnden FR and

Rosner R ApJ

ONeal D and Ne JE AJ

Young A Ajir F and Thurman G PASP

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

July

HU ISSN

NEW VARIABLE STARS IN ANDROMEDA

AND CASSIOPEIA

LENNART DAHLMARK

Residence Jeanne dArc A Avenue Ma joral Arnaud F Manosque France

 

This rep ort summarizes the results of a variablestar search in the  area cen

h m 

tered at Six similar elds have b een previously describ ed Dahlmark

The two earliest rep orts describ e the camera systems used

for the survey

Seventeen yellowblue plate pairs Ko dak aD GG lter and aO unl

tered were exp osed b etween and and fortyseven lms Ko dak TechPan

GG lter taken in the years to Six exp osures with a mm

Schmidt camera taken on TechPan without a lter were also examined and

used to prepare nding charts Ten plate or lm pairs were scanned for variables with

a blink comparator and with four stereo comparators used in tandem Magnitudes were

determined in a stereomicroscop e using comparison stars taken from the Guide Star Cat

alogue GSC Lasker et al The yellowlight magnitudes m shown in Table are

v

thus tied to the GSC northern magnitude scale and will b e systematically somewhat

brighter than standard Johnson V

In this eld twentysix variables were found one of which app ears only on two photos

taken on the same night Table shows p ositions and identications The co ordinates

were drawn mostly from the comprehensive USNOA catalogue Monet et al

00

one star app ears only in the GSC and another was estimated  using the Digitized

Sky Survey via the Go ddard SkyView facility The source of the p ositions is co ded in

column s as follows A USNOA G GSC v S SkyView

The elements of variation are collected in Table An asterisk by the star name

indicates a note at the b ottom of the table The lightcurve determinations are based

usually on sixtyeight magnitude estimates for each star From these the magnitude range

provisional variability type ep o ch of maximum and p erio d have b een determined For

several of the longp erio d variables it app eared that the variations though wellmarked

were not always consistent from cycletocycle The p erio d ranges found for such stars

from photos taken over a year interval are given in the last column The column b r

shows star colors from USNOA these are not well calibrated to any standard system

but serve to indicate in a qualitative way the sorts of stars involved

The star LD is listed as a p ossible dwarf nova candidate and deserves some dis

cussion It was observed on two simultaneous exp osures centered on Sept UT

JD at m The star is however not present on sixty other plates

v

00

from to A semiaccurate p osition reliable to within radius is shown

IBVS Figure

IBVS

in Table Arne Henden USNOUSRA kindly obtained BV photometry of the eld

on June UT with the USNOFlagsta meter telescop e The results are p osted

at ftpftpnofsnavymilpuboutgoingaahsequencedahldat There are no

blue ob jects in the immediate vicinity of the ob ject shown on the photographs The

ob jects closest to the candidate are three mag stars with B V color corresp ond

ing to K dwarfs or giants and some very faint galaxies Although no known asteroids

were in the eld at the time of the exp osures the p ossibility remains that the ob ject

photographed is a satellite glint of extremely short duration completely circular image

or some exotic ob ject as with recentlyobserved visible transients of gammaray bursts

0 0

The nder charts show a eld of  centered on the variables north is up and

east to the left

I would like to thank Arne Henden for his eort to identify LD in quiescence

Brian Ski Lowell Observatory aided in obtaining identications and precise p ositions

for the stars

Table Positions and identications LD LD

Name RA Dec s GSC IRAS Remarks

LD A

LD A

LD G

LD A

LD A

LD A FBS

LD A

LD A

LD

LD A

LD A

LD A

LD A

LD A

LD A

LD A

LD A at minimum on POSSI

LD A

LD A

LD S

LD A

LD A

LD A

LD A

LD A

LD A StM M

References

Dahlmark L IBVS No

Dahlmark L IBVS No

Dahlmark L IBVS No

Dahlmark L IBVS No

IBVS

Table Elements of variation LD LD

Name max min b r type ep o ch p erio d p erio d range

m JD days

v

LD I

LD Ia

d

LD SR

LD M

d

LD SR

LD M

LD M

LD L

LD UG

LD Ia

d

LD SR

LD M

LD E 

LD L

LD SR

d

LD M

LD M

LD SR

LD Lb

d

LD SR

LD L

LD Lb

LD M

d

LD M

LD Isa

d

LD M

Notes

d

LD blue from minima a p erio d of  is suggested

LD two maxima in exp ected but not observed

LD see text

h d

LD six minima observed eclipse duration p erio d is probably some fraction of

LD p erhaps a very long p erio d maxima observed in and but not

or one observation only however

Dahlmark L IBVS No

Dahlmark L IBVS No

Lasker B M Sturch C R McLean B J Russell J L Jenkner H Shara M M

Astron J

McGlynn T Scollick K and White N httpskviewgsfcnasagov see also

SkyView The MultiWavelength Sky on the Internet in McLean B J et al New

Horizons from MultiWavelength Sky Surveys IAU Symp osium No p

Kluwer

Monet D Bird A Canzian B Harris H Reid N Rho des A Sell S Ables H

Dahn C Guetter H Henden A Leggett S Levison H Luginbuhl C Martini

J Monet A Pier J Riep e B Stone R Vrba F Walker R USNO

A US Naval Observatory Washington DC see also httpwwwnofsnavymilprojectspmm

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

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July

HU ISSN

DISCOVERY OF A NEW MIRA VARIABLE

1 2

PK ABOLMASOV SYU SHUGAROV

1

Moscow City Palace for Youths Creativity Kosygina Str Moscow Russia

2

Sternberg Astronomical Institute Universitetskij Av Moscow Russia

email shugarovsaimsuru

Name of the ob ject

IRAS USNO A

Equatorial co ordinates Equinox

h m s  0 00

RA DEC J

Observatory and telescop e

cm astrograph in Crimea

Detector Photoplate

Filters None

Comparison stars See Fig

Check stars None

Transformed to a standard system B

pg

Standard stars eld used B band standard sequence in SA

Prieser

Availability of the data

Up on request

Type of variability M

Remarks

The variability of the star was discovered by S Antipin priv comm estimates

in interval JD show variations typical of Mira type variable with the

following light elements

d

JD  E

max

m m

The range of variability is

Acknowledgements

The authors would like to thank Dr VP Goranskij for his help and useful discussion

IBVS

Figure Finding chart and comparison stars

Figure Phased light curve Uncertain estimates are shown as op en circles v symbols represent

upp er limits

Reference

Prieser JB Naval Observ Publ vol XX p VI I Washington

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

July

HU ISSN

PHOTOMETRY OF THE OUTBURST OF U SCORPI I

SEI ICHIRO KIYOTA

Variable Star Observers League in Japan Azuma Tsukuba Japan

email skiyotaabrarcgojp

Name of the ob ject

U Sco

Equatorial co ordinates Equinox

h m s  0 00

RA DEC

Observatory and telescop e

cm Schmidt Cassegrain F

Detector Ap ogee AP CCD camera SITe SIAAB 

Filters JohnsonCousins BVR

c



Comparison stars GSC BD PPM V

B V based on Tycho catalog V R

calculated from B V value

Transformed to a standard system No

Availability of the data

Through IBVS Website as ttxt

Type of variability NR

Remarks

Patrick Schmeer rep orted the th recurrent outburst of U Sco m on

V

Feb Vsnetalert IAUC L Shaw rep orted that U Sco

reached the maximum of m at Feb IAUC I b egan to observe

V

this outburst immediately after maximum The lightcurve consists of parts the

st fast fading phase plateau around Mar the nd fast fading B V was

steeply decreasing after maximum but almost constant in the plateau phase The

plateau around days after the maximum was also rep orted at the outburst during

Sekiguchi et al

IBVS

Figure

Acknowledgements

I thank Dr Taichi Kato Kyoto University for useful discussion and advice

References

Schmeer et al IAUC

Sekiguchi K Feast MW Whitelo ck PA Overbeek MD Wargau W Jones JS

MNRAS

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

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July

HU ISSN

TIMES OF MINIMA OF ECLIPSING BINARIES

1 1 2

CLAUD H SANDBERG LACY KYLE MARCRUM CAFER IBANOGLU

1

Department of Physics University of Arkansas Fayetteville Arkansas USA

2

Astronomy Space Sciences Department Ege University Izmir Turkey

We rep ort times of minima of eclipsing binaries derived from photometric observations

made by CI at the Ege University Observatory in Turkey in Johnson B V lters and

at the University of Arkansas unltered CCD observations made by KM Helio centric

times of minima were estimated for each lter by using the metho d of Kwee and van

Woerden as adapted to a Macintosh computer The adopted time of minimum

was then the average over b oth lters for Ege data In all cases the times of minima in

dierent lters were concordant Uncertainties in the times of minima were estimated

from the values of standard error computed by the metho d and from dierences in times

derived from the various lters used In Table primary eclipses are designated as type

eclipses and secondary eclipses as type

Table

Star JD of Min Type Observatory Notes

WW Cam  Arkansas

V Cas  Arkansas

WW Cep  Arkansas

RW Lac  Arkansas

V Ori  Ege

BP Vul  Arkansas

 Arkansas

 Arkansas

Notes

The p erio d listed in the GCVS is almost exactly of the true p erio d found by

Torres from sp ectroscopic observations as  days From dates

of minima found in the eclipsing binary minima database at the web site

httpwwwoaujeduplkttindexhtml

we nd

Min I  n

From the zero ep o ch in the GCVS and our observation assuming a circular orbit con

sistent with published dates of minima we nd a p erio d of days in agreement

with the sp ectroscopic value The origin of the error in the GCVS p erio d is unknown

IBVS

Recent sp ectroscopic observations by Torres indicate that secondary eclipse

now o ccurs at a phase of  due to an eccentric orbit Our observed time of

secondary eclipse is in agreement with this prediction The eccentricity is approximately

based on the sp ectroscopic data

Our observation may b e combined with the observations of Lacy Fox to

yield an orbital p erio d of  days assuming a constant p erio d This

app ears to b e consistent with the p erio d listed in the GCVS but is more accurate

Figure A typical observation of a primary eclipse

References

Kwee KK and van Woerden H BAN

Lacy CHS Fox GW IBVS No

Torres G private communication

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

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July

HU ISSN

CCD LIGHTCURVES AND MINIMA TIMES

OF THE ECLIPSING BINARY RZ Cas

F J CLARKE T A LISTER

School of Physics Astronomy University of St Andrews North Haugh St Andrews Fife KY SS UK

email fjcstandacuk talstandacuk

The bright eclipsing binary RZ Cas has b een studied by many groups over the years

yet no completely satisfactory explanations for the systems o dd b ehaviour have b een

presented

Narrow band  A centred at A CCD observations were made with the m

James Gregory Telescope at the University of St Andrews Observatory on the nights of

December frames and January frames Relative magni

tudes were determined via dierential ap erture photometry using the star GSC

as a comparison GSC was used as a check star Times of minimum light for

the two primary eclipses observed were calculated via the metho d of bisecting chords and

were found to b e

JD :  :

JD :  :

The lightcurves obtained from our observations are shown in Figure It is clear that

RZ Cas displays b oth partial and total eclipses Several researchers have shown that

at b ottomed proles are unlikely to b e due to genuine total eclipses as they do not meet

the correct colour depth criteria Chambliss

Ohshima et al suggest that the at b ottomed proles are due to sup erp ositions

of eclipses and  Scuti type oscillations in the primary AV eg Maxted et al

The minute totality observed in January can b e explained as a  Scuti maxi

mum o ccurring near the time of minimum light This is compatible with the minute

p erio d Ohshima et al give for the  Scuti oscillations Rep orts in previous litera

ture of totalities up to minutes eg Arganbright et al are also agreeable with

this hypothesis Unfortunately our data are to o noisy to allow a signicant detection

of the  Scuti oscillations It also proved dicult to obtain an accurate estimate of the

relative depth of each eclipse due to a p o or determination of the maximum light level in

January

Further co ordinated monitoring of b oth minima times and eclipse proles is needed to

establish whether the changes in the light curves are p erio dic and if they are correlated

with any other phenomena in the system

Data were reduced at the St Andrews no de of the PPARC Starlink pro ject This

research made use of the SIMBAD database op erated at CDS

IBVS

Figure Eclipse lightcurves of RZ Cassiop eiae during December top and January

b ottom The lower January lightcurve has b een shifted by mags to make the diagram

clearer The change in prole b etween the the two data sets is apparent

References

Arganbright DV Osb orn W and Hall DS IBVS No

Chambliss C IBVS No

Maxted PFL Hill G and Hilditch RW Astron Astrophys

Ohshima O Narusawa S Akazawa H Mitsugu F Kawabata T and Ohkura N

IBVS No

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

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August

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TIMES OF MINIMA OF SOME SOUTHERN ECLIPSING BINARIES

1 2 3 4

Z KVIZ y M ZEJDA L KOHOUTEK J GRYGAR

1

Observatoire de Geneve Sauverny Switzerland

2

N Cop ernicus Observatory and Planetarium Kravhora Brno Czech Republic

3

Hamburg Observatory Go jenbergsweg Hamburg Germany

4

Institute of Physics Na Slovance Praha Lib e nCzech Republic

Moments of minima were derived for eight southern eclipsing binaries from photo elec

tric observations made with the seven channel photometer in the Geneva photometric

system by one of the authors Z Kvz in the years The photometer was

attached to the m Swiss reector op erating at the Europ ean Southern Observatory

La Silla Chile The reason for these observations was to study the interesting systems

esp ecially to investigate the p ossible p erio d changes of these short p erio d binaries see

eg Kvz Rufener Unfortunately Zdenek Kvz was not able to continue this

programme

The programme stars are listed in Table where the columns are as follows name

of the star brightness of the binary outside the eclipse and in the centre of the primary

minimum system of magnitudes used the letter P means photographic magnitudes and

the letter V denotes visual or photovisual magnitudes equatorial coordinates

and orbital elements M and P of the systems given in GCVS Kholop ov et al Samus

et al used in Table

The results are given in Table where HJD are the helio centric JD of the resp ective

minima together with their mean errors and n is the number of individual observations

used We also give the resp ective phases and the ep o chs see Table for the orbital

elements

The times of the minima were determined using the programme TINT Gaspani

based on the articial neural network The presented error is similar to the standard

deviation of the time of minimum The programme uses measurements made in all colours

and the Vmagnitudes were weighted separately from the magnitudes of six colour indices

The calculated phases of the minima dier signicantly from and resp ectively so

that small changes of p erio ds can b e exp ected with most of the mentioned stars

We wish to acknowledge the help of G Burki who gave us imp ortant information and

of A Gaspani for the p ossibility of using the programme TINT We thank the director

of the Geneva Observatory for supp orting the work of Z Kvzat La Silla

IBVS

Table List of programme stars

Brightness mag RA DEC M

Star Branch P days

Max Min I JD

U Col P

V Lep V

RS Lep V

RU Lep V

UX Men P

Phe V

BQ Sgr V

CW Vel V

Table Times of minima

Type of HJD

Star Error n Ep o ch Phase Note

minima

U Col prim normal min nights

sec normal min nights

sec

V Lep prim normal min nights

sec

RS Lep prim

sec

RU Lep prim

prim

prim

prim

prim normal min nights

sec normal min nights

UX Men prim

Phe prim normal min nights

sec

sec normal min nights

BQ Sgr prim normal min nights

sec normal min nights

CW Vel prim normal min nights

sec normal min nights

The error given in TINT a version of TINAGEL is very similar to a standard deviation and it

describ es the true uncertainty of t b etter than only the statistical prop erties of the data set would do

References

Gaspani A private communication

Kholop ov PN ed et al Samus N N ed et al General Catalogue of Variable

Stars electronic edition v ftpftpsaimsusupubgroupsclustersgcvsgcvs

KvzZ Rufener F IBVS No

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

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August

HU ISSN

RZ CEPHEI PERIOD VARIATION

IOAN TODORAN RODICA ROMAN

Astronomical Observatory ClujNap o ca Romania

The variability of RZ Cephei was discovered by Leavitt in This is an RR type

C

star and its observation is imp ortant for at least three reasons i the p erio d variability

ii a premaximum hump in the light curve and iii its high space velocity For a more

detailed historical information we recommend the article written by Cester and Todoran

Here only the p erio d variability is concerned In Table we rep ort a series of ob

served maxima maxima observed by Alania and Abuladze and maxima

observed by Todoran The times of maxima were determined by Roman

Even if the observations are p erformed with photo electric photometers having in view

the varying shap e of the light curve in the vicinity of its maximum Pogsons metho d and

mean light curve were used in order to determine the helio centric times of maxima The

results are given in Table Here the corresp onding O C dierences were computed by

using the linear ephemeris

d

Max HJD  E

and could b e aected by the variability of the corresp onding light curve

In their study referring to the p erio d variation Cester and Todoran p ostulated

a cycle of years while Todoran has written we can say that RZ Cephei is at

least a triple p erio dic variable star

Now in order to have a general image ab out p erio d variation of RZ Cephei we have

also used the observed maxima listed by Todoran Cester and Todoran

Maintz and Seifert

For all the ab ove mentioned maxima the O C residuals are displayed in Fig

where the cyclic variation is evident but at least a critical remark could b e relevant The

amplitude of the p erio d variation is ab out twice the length of the p erio d We consider

that such a situation is determined by the fact that we have here in the same time two

unknown parameters the length of the p erio d and the corresp onding cycle number E

Therefore it is evident that RZ Cephei must b e observed in the future and the p erio d

variation to b e connected with the changes observed in the shap e of the light curve

IBVS Figure

IBVS

Table Observed maxima of RZ Cephei

HJD n O C E Observer

d

Alania Abuladze

d

Alania Abuladze

d

Alania Abuladze

d

Alania Abuladze

d

Alania Abuladze

d

Todoran

d

Alania Abuladze

d

Alania Abuladze

d

Todoran

d

Todoran

d

Todoran

d

Todoran

d

Todoran

d

Todoran

d

Todoran

d

Todoran

d

Todoran

d

Todoran

d

Todoran

d

Todoran

d

Todoran

d

Todoran

d

Todoran

d

Todoran

d

Todoran

References

Alania JF Abuladze OP Bull Abastum Astrophys Obs

Alania JF Abuladze OP Bull Abastum Astrophys Obs

Cester B Todoran I IBVS No

Cester B Todoran I Mem So c Astron Ital

Maintz G BAVM No

Seifert K BAVM No

Todoran I IBVS No

Todoran I Multiple Periodic Variable Stars IAU Collo quium No ed WS Fitch Vol AkademiaiBudap est p

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PHOTOMETRY OF THE  SCUTI STAR HR

LIU YY

Beijing Astronomical Observatory Chinese Academy of Sciences Datun Road A Chaoyang District

China email lyyclassbaoaccn

HR was discovered to b e a Scuti star by Breger Its rep orted p erio d

is days No observation has b een done since that time This star has a Del like

sp ectrum Cowley et al and is the primary of a visual binary system Moreover

the pulsating variable HR also b elongs to a sp ectroscopic binary Stromgren v and

y rapid photometry was carried out with the cm reector during and January in

at Xinglong of Beijing astronomical observatory Chevreton sixchannel photometer

Michel was used This system allows a highsp eed data acquisition with go o d

accuracy one record p er second Light from the stars is divided into v and y parts by

means of a dichroic lter so that two bands can b e simultaneously monitored through two

identical photomultipliers Therefore four of the channels are used for the program and

comparison stars in v and y resp ectively The sky background was obtained by the other

two channels using standard v and y lters separately The observational eld is around

arcmin The comparison star was SAO no variability has b een rep orted on

it Finally successive day data were obtained Due to bad weather data on Jan

was excluded in v dataset Light curve of last night is not p erfect but the variability is

obvious

The instrumental magnitude of the variable can b e obtained by dividing their photon

counts after removing the sky background Eect of resp onse for the dierent channels

has b een taken into account A p olynomial tting was applied to remove the eects from

intrinsic variability transparency turbulence and the instrumental drift caused by the

temp erature changes of photomultipliers The nal light curves in two lters are shown

in Fig and These data have b een averaged so that each p oint represents one minute

The pulsation p erio d was analyzed through Fourier transform to v band data using

co de MFA Hao b ecause larger scatter exists in y A frequency f cd is

found It ts b oth v and y datasets well as displayed in Figure and Sp ectral window

and p ower sp ectra are outlined in Figure Table lists the relevant parameters

HR was rstly observed almost thirty years ago the hours data resulted in an

estimation of frequency b eing cd that cannot b e approved by new observation

This value fails to interpret new light curves Its amplitude has also decreased From

the Hipparcos observation absolute magnitude of HR is derived as M

v

Eective temp erature and gravity are obtained by means of the photometric calibration

according to Domingo Figueras giving log T log g The Q

e

value was calculated Q B C implying a nonradial mo de The phase

IBVS

Figure Observed light curves of HR in v band The solid lines are the leastsquares t with the

frequency listed in Table The abscissa is HJD and the ordinate in mag

Table Prop erties of the light curve of HR in v and y bands

frequency Amp v Phase v Amp y Phase y

cd mmag rad mmag rad

    

shift and amplitude ratio can b e used to have insight ab out the pulsation mo des However

considering the short data base and low amplitude the phase shift is uncertain and may

not give meaningful explanation In fact unknown frequency can b e hidden in the light

curves a second frequency around cd is probably an intrinsic one More observa

tion covering long time base is strongly needed to conrm it and then to understand the

IBVS

Figure Same as Fig but in y band

IBVS

Figure Sp ectral window and p ower sp ectra of HR in v band

pulsation character of this star

This work was supp orted by the grant of National Natural Science Fundation of China

NSFC

Acknowledgement The author is very grateful to Drs F Figueras and A Domingo for

providing their photometric calibration co de

References

Breger M AA

Cowley A Cowley C Jaschek M et al AJ

Domingo A Figueras F AA

Hao J Pub Of the Beijing Astro Obs

Michel E Belmonte JA Alvarez M et al AA

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

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August

HU ISSN

IRAS A NEW MIRA VARIABLE

1;2 3

B HASSFORTHER U BASTIAN

1

Ringstr Heidelb erg Germany email b elaaolcom

2

Bundesdeutsche Arb eitsgemeinschaft f ur Veranderliche Sterne eV BAV Munsterdamm D

Berlin Germany

3

Astronomisches RechenInstitut Monchhofstr Heidelb erg Germany

email sixurzuniheid el b ergde

The Stardial pro ject of the University of Illinois at UrbanaChampaign provides a

sky patrol of a declination band just south of the equator using a driftscan rob otic

CCD camera All the images are immediately made available on the worldwide web

under httpwwwastrouiucedustardial While blinking Stardial frames in a search

for new variables the star IRAS USNOA lo cated at

h m s  0 00

J from USNOA was found to vary b etween ab out

and fainter than in unltered CCD magnitudes

The Stardial lightcurve from all usable frames collected over observing seasons

indicated Miratype variability with a p erio d of ab out days Fig shows p ositive mag

nitude measurements relative to GSC as solid diamonds and upp er limits from

nondetections as very small triangles There is a clearcut maximum around JD

and an incomplete one at ab out JD In b etween a minimum is indicated by

a decline around JD and a rise around JD The minimum itself is

indicated by the large number of nondetections small symbols around JD In

addition there is a rise around JD given by a group of nondetections followed

by a group of p ositive observations

This interpretation of the Stardial data is corrob orated by frames from The Am

ateur Sky Survey TASS another public CCD sky patrol pro ject see httpwwwtass

surveyorg I band magnitudes derived from the frames are displayed as crosses

in Fig Due to the larger optics compared to Stardial the TASS data give p ositive

observations even close to the minimum

From Fig the following rough ephemeris can b e derived

JD Max  E

Acknowledgements This research made use of the SIMBAD data base op erated by

the CDS at Strasb ourg France

IBVS

Figure Lightcurve of IRAS Symbols are explained in the text

COMMISSIONS AND OF THE IAU

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HU ISSN



LS II A NEWLY RECOGNIZED CLASSICAL Be STAR

AS MIROSHNICHENKO KS KURATOV TA SHEIKINA DB MUKANOV

1

Ritter Observatory Dept of Physics Astronomy University of Toledo Toledo OH USA email

anatolyphysicsutoledoedu

2

Fesenkov Astrophysical Institute Kamenskoye plato Almaty Kazakhstan

3

AlFarabi Kazakh National University Almaty Kazakhstan



LS i i was discovered by Sto ck et al as a p ossible luminous earlytype

star with emission in the H line Later it was listed in the Henize catalog of

emissionline stars as Hen Pesch estimated its sp ectral type as B ia or

B v with less likelihoo d from his UBV photometry see Table which also implies

m

the interstellar extinction A  assuming no circumstellar contribution Allen

V

m m

obtained nearIR photometry of the star H K These data indicate a

very weak nearIR excess radiation see Fig taking into account the ab ove A a total

V

toselective interstellar extinction ratio R and intrinsic colorindices for the ab ove

sp ectral types Stra jzhys This excess can b e explained by freefree emission of the

m

circumstellar gas or of a faint co ol companion Its weakness and shap e E 

V K

m

dereddened H K rules out the presence of hot dust around the star



Dong Hu identied LS i i with the IRAS PSC source

However the IRAS uxes detected at and m and Jy resp ec

tively imply a very strong ux rise b etween and m which is inconsistent with the

assumption ab out a latetype companion see Fig Such a rise might b e due to the

radiation of dust with the highest temp erature of nearly K Moreover a steep de

crease of these IRAS uxes with wavelength is consistent with either a small extent of the

dusty structure or with a dierent illuminating source for the dust The rst suggestion

along with the absence of the hot dust leads to a conclusion that the dust is concentrated

in a rather thin remote shell while the second one p oints that either the optical ob ject is

a binary system or it is not asso ciated with the IRAS source

00

The et al p ointed out that there is a oset b etween the optical p osition



of LS i i and that of the IRAS source This is well outside the IRAS p ositional

00 00 

error ellipse which has ma jor axes of and and a p osition angle of A faint

star that is lo cated very close to the p osition of IRAS is seen in the Space



Telecope Institute Digital Sky Survey image of a eld around LS i i It seems to

b e a more appropriate optical counterpart of this IRAS source The midIR sp ectrum

of IRAS taken by the IRAS LowResolution Sp ectrometer LRS shows a

weak emission feature at m Olnon et al which is probably due to the SiC



dust particles usually observed in the sp ectra of carb on stars Therefore LS i i and

IRAS are most likely dierent sources

IBVS



The simultaneous U B V RI observations of LS i i in the Johnson photometric

system were obtained with two meter telescop es at the Assy and TienShan Obser

vatories of the Fesenkov Astrophysical Institute in Kazakhstan equipp ed with a two

channel photometerp olarimeter Bergner et al b etween June and August

00

through the diaphragm Table Its brightness varies with an amplitude of

m m

 in the V RI bands while it reaches in the U band Such a b ehaviour might b e

due to freeb ound emission of the circumstellar gas which gives the strongest contribution

shortward of the Balmer jump and manifests itself by the p eculiar sp ectrum see b elow

The averaged colorindices U B and B V are consistent with those of a reddened B

m

giant or dwarf A  R which displays an excess radiation longward of

V

m m

m The latter increases from ab out in the Rband to in the K band ac

cording the data by Allen It can b e explained by freefree emission of the envelope

as in classical Be stars eg Dougherty et al



Table Photometric observations of LS i i

JD V U B B V V R R I

a

a

data from Pesch

The sp ectroscopic observations were obtained at the meter telescop e of the Russian

Academy of Sciences with a photo electric TVscanner Balega et al on July

in the sp ectral regions and A with a resolution of A The most

prominent features in the sp ectrum are a doublep eaked H emission Fig and Fe i i

absorption lines The H line is mostly lled in with emission while H and H show only

weak signs of it Other emission lines which are seen in the sp ectrum can b e identied

with Fe i transitions usually blends of several lines The Na i D and Si i i and

A absorption lines certainly contain circumstellar contribution as their equivalent

width ratios are dierent from those of pure interstellar and photospheric and

resp ectively The observed diuse interstellar bands at and A are rather strong

and are consistent with the reddening derived ab ove from the photometric data

The strong inuence of the circumstellar material makes it dicult to estimate the

MK type of the star from our sp ectral data The observed H line wings are consistent

with the theoretical ones for the temp eratures not higher than K that corresp onds

to a B sp ectral type Since the H emission line is not very strong and hardly aects

the Balmer jump Doazan we can assume that our photometric estimate of the

ob jects MK type is correct

The H line prole and strong Fe i i absorption lines are similar to those of classical

Beshell stars where they are formed in a dense circumstellar disk viewed at a high

inclination angle close to edgeon Hanuschik The observed ratio of the H p eak

intensities V R is also seen in many classical Be stars and is thought to b e due to

IBVS

rotating onearmed density waves in the disk eg Okazaki The optical brightening

accompanied with the blueing observed in August two last lines in Table may b e

due to the shell strengthening which is usual for classical Be stars eg Doazan



Figure The dereddened SEDs of LS i i constructed from the averaged U B V RI H K

photometric data lled circles along with that of IRAS lled squares IRAS

photometry crosses IRAS LRS sp ectrum A Kurucz mo del atmosphere for T K

e

and log g is shown by a solid line

The separation b etween the H emission p eaks  km s implies a rotational

velocity of the envelope of at least km s if one assumes that rotation is the main

mechanism of the line formation Subtraction of the photospheric prole from the observed

H line prole reveals a doublep eaked emission similar to that in the H line

If we suggest a typical luminosity of a late Btype classical Be star for the ob ject

log L L  eg Zorec Briot a distance of  kp c can b e derived An

b ol

assumption that the ob ject is a sup ergiant is not consistent with the derived sp ectral type

and intrinsic colorindices of the star Furthermore the presence of a disklike gaseous

envelope is a feature of Be sup ergiants Zickgraf et al which also exhibit a



strong nearIR excess not seen in LS i i Balmer line proles similar to those of the

ob ject also display premainsequence Herbig AeBe stars Finkenzeller Mundt

However such a strong emissionline sp ectrum in these stars is usually acompanied by



a noticeable nearIR excess that rules out the premainsequence nature of LS i i

The collected observational data do not allow us to consider other p ossible options eg

binary system with dierent types of the secondary comp onent



Thus b oth photometric and sp ectroscopic prop erties of LS i i suggest that it is

most likely a classical Beshell star Its emission in the H line is one of the strongest

among those of Be stars with nearly similar sp ectral types It is similar to that of Pleione

during its shell phase Doazan New photometric and sp ectroscopic variations of

IBVS



Figure The H line prole in the sp ectrum of LS i i The helio centric velocity is given in

km s the intensity is normalized to the continuum



LS i i are therefore exp ected in the future The IRAS source is most

likely asso ciated with a co ol nearby star

References

Allen DA MNRAS

Balega II Vereschagina RG Markelov SV et al Izvestia Spec Astroph

Obs

Bergner YuK Bondarenko SL Miroshnichenko AS et al Izvestia Glavn

Astron Obs v Pulkove

Dong YS Hu JY Chin AA

Doazan V in The B Stars with and without Emission Lines AB Underhill V

Doazan eds NASA SP

Dougherty SM Taylor AR Clark TA AJ

Finkenzeller U Mundt R AAS

Hanuschik RW Proc IAU Symp eds LA Balona HF Henrichs and

JM Le Contel Kluwer Acad Publ p

Henize KG ApJS

Kurucz RL Smithsonian Astrophys Obs CDROM No

Okazaki AT PASJ

Olnon FM Raymond E and IRAS Science Team AAS

Pesch P ApJ

Sto ck J et al Luminous Stars in the Northern Milky Way Part i i

Stra jzhys V in Multicolor Photometry of Stars Vilnius Mokslas

ThePS de Winter D PerezMR AAS

Zickgraf FJ Wolf B Stahl O et al AA

Zorec J Briot D AA

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

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August

HU ISSN

RISE FROM THE LOW STATE OF THE BINARY V SAGITTAE

1 2

V SIMON S SHUGAROV

1

Astronomical Institute Academy of Sciences Ondrejov Czech Republic email simonasucascz

2

Sternberg Astronomical Institute Moscow State University Universitetsky Prosp ect Moscow

Russia email shugarovsaimsuru

d

V Sge is a p eculiar eclipsing binary P Herbig et al The sp ec

orb

trum consists of a hot continuum with strong emission lines and resembles the type WN

Recently there have b een accumulated several lines of evidence existence of the high

excitation emission lines Patterson et al Xray variations Greiner and van Teesel

ing the character of the longterm activity Simon and Mattei which strongly

supp ort the mo del of the mass accreting white dwarf primary from a massive companion

originally suggested by Williams et al V Sge app ears to b e a promising candidate

for the sup ersoft Xray source SSXS Steiner and Diaz see van den Heuvel et al

for denition of SSXS

V Sge displays very strong photometric activity Herbig et al Simon

Rob ertson et al Simon and Mattei The character of the activity changed

from relatively isolated outbursts seen in s to alternating high HS and low LS

states separated by transitions often of signicantly shorter duration than the states

HSLS b ehaviour is the most common kind of activity in V Sge during the last more than

ab out years

We rep ort on UBV observations of the rise from LS to HS which o ccurred in August

The measurements were obtained with the mm Cassegrain telescop e at

Moscow Observatory of Sternberg Astronomical Institute The star V B V

0 0

U B lo cated N E from V Sge was used as the comparison star The

0 0

check star was V B V U B N W from the variable

Series of densely spaced measurements covering up to several hours were secured in most

nights

This rise was suciently slow to b e resolved it gave a rare opp ortunity to follow

variations of the light curve through the LSHS transition The course in V lter can

b e seen in Fig a The asso ciated U B and B V indices are included in Fig b c

The dots in Fig b c are the individual measurements while the empty circles denote the

nightly means The horizontal lines in Fig b and c mark the average color index for

the whole transition the mean U B and B V b eing and resp ectively

On average the p oints in Fig c are grouping at progressively bluer B V index as the

system brightens during the transition while U B do es not exhibit any noticeable trend

Examination showed that orbital variations of the color if any are signicantly smaller

than those invoked by the longterm activity

IBVS

Figure Rise from the low to the high state of V Sge Observations obtained within a given night

dots are connected by line The empty circles in Fig b and c mark the nightly means the horizontal lines denote the mean color index for the whole transition

IBVS

No previous color changes for the LSHS transition in V Sge have b een published

Only Herbig et al listed UBV observations of an outburst which o ccurred in the

b eginning of sixties they therefore represent a kind of activity which has changed during

the last decades see Simon and Mattei Both average color indices determined

from our data agree within mag with those of Herbig et al Also the fact

that B V decreases by  mag in the upp er part of the rise to HS is similar to the

b ehaviour of this index at the p eak of the outburst observed by Herbig et al It

therefore app ears that although the character of the activity in V Sge has changed since

s the colors and their variations with the brightness level remained similar

Acknowledgements This research has made use of NASAs Astrophysics Data System

Abstract Service Investigation of cataclysmic variables with Xray emission is partly

supp orted by the pro ject KONTAKT ME by the Ministry of Education and Youth

of the Czech Republic This study was also supp orted in part by the Russian Foundation

for Basic Research and the Council of the Program for the Supp ort of Leading Scientic

Schools through grants No and

References

Greiner J van Teeseling A AA L

Herbig GH Preston GW Smak J Paczynski B ApJ

Patterson J Kemp J Shambrook A Thorstensen JR Skillman DR Gunn J

Jensen L Vanmunster T Shugarov S Mattei JA Shahbaz T Novak R

PASP

Rob ertson JW Honeycutt RK Pier JR AJ

Steiner JE Diaz MP PASP

Simon V AAS

Simon V Mattei JA AAS accepted

van den Heuvel EPJ Bhattacharya D Nomoto K Rappap ort SA AA

Williams GA King AR Uomoto AK Hiltner WA MNRAS

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

August

HU ISSN

CCD PHOTOMETRY OF BF ERIDANI

A LOWAMPLITUDE DWARF NOVA

T KATO

Dept of Astronomy Kyoto University Kyoto Japan email tkatokusastrokyotouacjp

BF Eri was originally classied as a slowly varying variable star The fourth edition

of General Catalogue of Variable Stars listed it as a semiregular variable star with a

range of pg However the likely identication of the Einstein survey source ES

with BF Eri Elvis et al and optical sp ectroscopy Schachter et al

led to the correct identication as a cataclysmic variable The source was also detected

during the course of the ROSAT AllSky Survey RXS J RXP J

and p ointed observations WGA J The ROSAT identication of

the Einstein source also led to an identication as a cataclysmic variable of unknown type

Chisholm et al Indep endently noting the identication of BF Eri with the ROSAT

source the VSOLJ Variable Star Observers League in Japan and the author started

visual and CCD monitoring of this ob ject The rst result of visual monitoring Watanabe

led to a conclusion that BF Eri is a dwarf nova with a recurrence p erio d of

d and the range of m I here rep ort longterm and shortterm variation by

v

CCD photometry

The observations were done using an unltered ST camera attached to the Meade

cm SchmidtCassegrain telescop e The exp osure time was s The images were

TM

darksubtracted atelded and analyzed using the Java based ap erture photometry

package developed by the author The dierential magnitudes of the variable were mea

sured against GSC USNO r magnitude whose constancy was conrmed

by comparison with GSC USNO r magnitude Table summarizes nightly

averaged magnitudes relative to GSC

The longterm light curve of BF Eri is shown in Figure Each p oint represents a

nightly averaged magnitude with an error bar indicating the standard error The initial

part of the light curve corresp onds to the nal declining stage of the second outburst

rep orted by Watanabe Around JD February another distinct

brightening outburst was observed The outburst smo othly decayed in the following

ve days with an average rate of mag d The combination of overall CCD obser

vation and the visual monitoring Watanabe indicates that the typical amplitude

of outbursts is  mag The discovery observation may indicate the amplitude can b e

as large as mag The overall b ehavior of this star resembles those of lowamplitude

dwarf novae or of some NLtype variables The likely existence of outburst p erio dicity

Watanabe prefers the dwarf nova interpretation

IBVS

Table CCD observation of BF Eri

a a b c d

JD start JD end N mag error

a

JD

b

Number of frames

c

Magnitude relative to GSC

d

Standard error of nightly average

IBVS

1.5 BF Eri

2 Relative magnitude

2.5

190 200 210 220 230 240 250 260

JD - 2451000

Figure Longterm light curve of BF Eri

1.8 BF Eri (1999 Feb 6)

2

2.2 Relative magnitude 2.4

2.6

216.02 216.04 216.06 216.08 216.1

HJD - 2451000

Figure Shortterm variability on February

IBVS

Figure illustrates a representative shortterm light curve of BF Eri where each p oint

represents a single measurement Slow mo dulations with a typical timescale of hours

usually exist with p ossible sup erp osition of shorter timescale mo dulations However

Fourier analysis of the longer data sets after subtracting the nightly trend did not yield

a stable p erio dicity b etween d and d

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture and Sp orts

References

Chisholm J R Harnden F R Jr Schachter J Micela G Sciortino S Favata F

AJ

Elvis M Plummer D Schachter J Fabbiano G ApJS

Schachter J Remillard R Saar S Favata F Sciortino S Barb era M ApJ

Watanabe T VSOLJ Variable Star Bul letin in press also available from httpwwwkusastrokyotouacjpvsnetMailvsnetmsghtml

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

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August

HU ISSN

NEW VARIABLE STARS DISCOVERED IN THE MISAO PROJECT

I MisVMisV

1 2

SEI ICHI YOSHIDA KENICHI KADOTA

1

MISAO Pro ject Miyawada Fujishiromachi Kitasomagun Ibaraki Japan

email seiichimuraokainfowasedaacjp

2

MISAO Pro ject Koshikiya Ageo City Saitama Japan

email kenickastroartscojp

This rep ort describ es the new variable stars MisVMisV discovered in

the course of the MISAO Pro ject

The goal of the MISAO Pro ject standing for Multitudinous Imagebased Skysurvey

and Accumulative Observations is to discover new celestial ob jects or to obtain photo

metric data from multitudinous astronomical images The details are describ ed on the

MISAO Pro ject Home Page

httpwwwinfowasedaacjpmuraokamembersseiichimisao

Here we use only the unltered CCD images taken by KenIchi Kadota in Ageo City

Japan for new variable stars survey The images were taken b etween December and

June mainly with a m f reector and m f reector The CCD chip

is Ko dak KAF

We used the PIXY system for the survey The PIXY system standing for Practical

Image eXamination and Innerob jects Identication system is developed and distributed

by Seiichi Yoshida It automatically detects stars from images measures the p osition and

magnitude identies them with known variable stars in the GCVS etc and outputs can

didates of new ob jects and new variable stars After the PIXY system output candidates

of variable stars Seiichi Yoshida and KenIchi Kadota manually checked each of them on

our CCD images Then we found ob jects are really variable and previously unknown

We judged only ones whose variability is surely evident as new variable stars

Here is the list of new variable stars Table The p osition and magnitude are

measured with USNOA catalog Because the pixel size is arcsecpixel or

arcsecpixel astrometric errors may sometimes exceed arcsec except for stars identied

with data in the Guide Star Catalogue or the USNOA catalog The magnitude is

based on a preliminary V magnitude calculated from R and B magnitude in the catalog

based on Taichi Katos equation

V R B R

So the value is somewhat shifted from magnitude in the standard system But it do es not

matter for range of variability Because they were observed on a few nights the p erio d is

quite uncertain The preliminary type is attached for some ob jects observed for several

IBVS

nights Most of them were observed twice or more during a few month interval and the

magnitude dierence is over mag so most of them will b e long p erio d variable stars M

or SR type The latest list b eing up dated with our followup observations is available

at the MISAO Pro ject Home Page The nding charts are available electronically as

fnnneps where nnn refers to the serial number assigned to the star in the rst

column of Table

We would like to thank Dr Taichi Kato for checking known variable stars his advice

on type of variability and many informative discussions

References

Seiichi Yoshida Practical Image Examination and InnerObjects Identication System in

preparation for PASP

Taichi Kato

httpwwwkusastrokyotouacjpvsnetMailvsnetchatmsghtml

Table List of New Variable Stars

Unltered

CCD Mag

Type Identied with Co de RA J Decl

Max Min

h m s  0 00

MisV M

MisV E GSC

USNO

MisV SR

MisV M

MisV USNO

MisV

MisV USNO

MisV

MisV USNO

IRAS

MisV USNO

MisV SR IRAS

MisV SR IRAS

MisV

MisV

MisV USNO

MisV

MisV M

MisV

MisV IRAS

MisV

IBVS

Table cont

Unltered

CCD Mag

Type Identied with Co de RA J Decl

Max Min

h m s  0 00

MisV

MisV

MisV

MisV

MisV

MisV

MisV

MisV

MisV

MisV M USNO

MisV USNO

MisV

MisV

MisV

MisV USNO

MisV

MisV

MisV

MisV

MisV USNO

MisV GSC

USNO

IRAS

MisV SR IRAS

MisV SR

MisV SR

MisV USNO

MisV SR

MisV SR

MisV IRAS

MisV

MisV SR

MisV SR USNO

MisV USNO

MisV

MisV

MisV

MisV IRAS

MisV

MisV

MisV

MisV SR

IBVS

Table cont

Unltered

CCD Mag

Type Identied with Co de RA J Decl

Max Min

h m s  0 00

MisV M

MisV

MisV

MisV SR

MisV SR

MisV

MisV SR

MisV

MisV IRAS

MisV M USNO

MisV SR USNO

MisV

MisV L USNO

MisV IRAS

MisV IRAS

MisV M IRAS

MisV IRAS

MisV USNO

MisV

MisV

MisV

MisV USNO

MisV USNO

MisV SR USNO

MisV SR

MisV SR

MisV SR

MisV SR

MisV

MisV IRAS

MisV SR USNO

MisV IRAS

MisV SR IRAS

MisV IRAS

MisV

MisV USNO

MisV

MisV

MisV

MisV

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HU ISSN

THE LIGHT CURVES OF SX Phe STARS IN NGC

E PORETTI

Osservatorio Astronomico di Brera Via E Bianchi I Merate LC Italy

Email p orettimeratemiastroit

Recently attention has b een paid to short p erio d P d pulsating stars lo cated

in globular clusters Poretti reanalyzed the data collected by the OGLE team

on new SX Phe stars in Centauri Fourier decomp osition extended the P

relationship toward shorter p erio ds The existing progression Antonello et al

Poretti et al is continued in a natural way even if some p eculiarities were found

a group of deviant p oints around d a change in the slop e around d and a

single unusual light curve OGLEGC P d

Thompson et al rep orted on CCD photometry of new variable stars in the

eld of another globular cluster NGC Among them there are three new SX Phe

stars Their light curves lo ok very dierent from each other and the classication of

their prop erties pulsation mo de membership in the cluster are considered to b e

problematic It is interesting to examine the prop erties of their light curve to verify the

results obtained in Cen

First we conrmed the previously found p erio ds using an indep endent frequency anal

ysis we note that the sp ectral window is go o d since aliases at  c d are b elow the

of the central p eak Then we applied the Fourier decomp osition Three V light curves

deserve attention

Star P d The full amplitude is only mag but the light curve is

nd

very well dened A order t leaves a residual of only mag and an accurate

value can b e derived  rad in excellent agreement with the exp ected value

Contrary to the doubts expressed by Thompson et al there is no problem in

considering this star as one which pulsates in its fundamental mo de

Star P d Its value is well dened  rad and very

rd

close to the exp ected one The large amplitude allows a order t The value

 rad is in excellent agreement with the values rep orted by Poretti

Table which in turn are very coherent with those of largeamplitude galactic variables

Star P d It is the most interesting star since its p erio d falls in

the region where Poretti found some deviant values Unfortunately the light

curve has a fullamplitude of only mag and the derived Fourier parameters are a little

uncertain However the value is actually higher than exp ected 

Fig shows the values of the pulsating stars found in the Galaxy op en squares

with d P d corresp ond to CY Aqr ZZ Mic and V Tau in Cen lled

dots and in NGC crosses The p oints related to OGLEGC and OGLEGC

IBVS

Figure The P plot for pulsating variables observed in the Galaxy squares in Cen lled

21

dots and in NGC crosses Error bars are rep orted for the small amplitude stars suggesting two

separated groups at P d

are omitted see Poretti for discussion From Fig it is quite evident that we

nd pulsating stars with only P d in globular clusters As an additional example

the shortest p erio d observed in the OGLE database is d V in the BW eld

Udalski et al

It should b e noted that the disp ersion of the values for stars with P d is

much larger than for stars with P d Of course this can result from the larger

errors related to the small amplitudes less than mag of the shortest p erio d variables

error bars are shown in Fig for this purp ose However the working hypothesis of two

dierent pulsation mo des fundamental or rst overtone radial mo des nonradial mo des

should b e fruitfully investigated on the basis of new more accurate data

Acknowledgements The author wishes to thank Ian Thompson and Janusz Kaluzny

for putting the NGC data at his disp osal

References

Antonello E Broglia P Conconi P Mantegazza L AA

Poretti E AA

Poretti E Antonello E LeBorgne JF AA

Thompson I Kaluzny J Pych W Krzeminski W astroph

Udalski A Olech A Szymanski Kaluzny J Kubiak M Mateo M Krzeminski W

Acta Astronomica

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HU ISSN

DIFFERENTIAL UBV PHOTOMETRY OF TWO CP STARS

Her AND Her

M ZBORIL J BUDAJ

Astronomical Institute TatranskaLomnica Slovakia email zb oriltask buda jtask

The chemically p eculiar star Her Her HR HD HIP SAO

Bp HgMn m was selected from the pap er of Catalano to inves

V

tigate the photometric p erio ds amongst HgMn sp ectroscopic binaries The ob ject is an

SB system with long orbital p erio d of days Aikman Winzer found

no evidence of signicant photometric variations Rakosch and Fiedler rep orted

d

on p erio d in the U lter with the amplitude mag but state that the star is

constant in B and V lters ab ove the semiamplitudes and mag resp ectively

based on UBV observations made in season Since then no undoubtful p erio d

d

icity has b een rep orted and esp ecially as concerns Catalano and Renson for

d

example give the Rakosch and Fiedler p erio d with question mark Harmanec

et al mentioned that there might b e some microvariability but not with the p erio d

after Rakosch and Fiedler Recently very tiny light variations with the amplitude

mag from to mag were rep orted by ESA in the Hipparcos data

However Adelman argues that the star is constant the amplitude contains the

contribution from noise for example

The chemically p eculiar star Her Her HR HD HIP SAO

BI I Ip HgMn m was used as comparison star by Rakosch Fiedler

V

and no variability has b een rep orted as yet including the Hipparcos observations

Stellar sp ectra of b oth stars were studied and p erhaps rep orted rstly by Slettebak

The UBV observations have b een carried out at Stara Lesna observatory with the

photoelectric photometer attached to m reector The comparison stars were already

mentioned Her standard and SAO check HD A m and

V

the observations were made in the sequence times comp times var times

check Each observation of the star was followed by recording the sky background The

observations were corrected for dierential extinction The standard star was identical

with that from Rakosch and Fiedler The observations were made in overall number

of nights covering the season January up to September Duration of a typical

night run was hour

The weather conditions enabled us to obtain go o d observations needed for the search

for p erio dicities of low amplitudes around mag as much as nights on average

Tables and list the instrumental magnitudes in each lter The night averages are given

with corresp onding r ms errors and column entitled n stands for number of individual measurements in particular night

IBVS

Table Her Her JD

JD U  n JD B  n JD V  n

Figure Phase diagram based on equation U lter Her Her

Figure Phase diagram based on equation U lter Her Check

IBVS

Table Her Check JD

JD U  n JD B  n JD V  n

Figure Phase diagram based on equation B lter Her Her

Figure Phase diagram based on equation B lter Her Check

IBVS

We primarily fo cused the eort to verify the p erio d of days resulting from the

ephemeris by Rakosch and Fiedler

JDU  E

min

Figures give magnitude dierences vs phase in U and B lters resp ectively We did

not nd any outstanding p erio d and the star seems to b e constant The p ower sp ectra

enabled us to put the following constraints on the constancy the semiamplitudes of

the variable star mmag in U B and V lters resp ectively Consequently we

d

cannot conrm the p erio d suggested by Rakosch and Fiedler Using Her

as standard star might not b e a go o d practice but it was motivated by comparison stars

option by Rakosch Fiedler As a byproduct we can state that the same constraints on

the constancy are also valid for another CP star Her this time in agreement with the

Hipparcos satellite observations

Our UBV observations questioned the variability of Her and suggest light constancy

b eyond mag limit in the season The same limit for light variability go es

for comparison star and another CP star Her Similarly to Adelman Adelman et

al and Zb oril and Buda j we added another star to a list of constant HgMn

stars ab ove mag limit which were originally rep orted as variable stars However

we still welcome new observations since i we cannot exclude low amplitude variability

b elow mag such as that rep orted by ESA ii the star was rep orted by Bab co ck

as magnetic star and iii the star might have changed the p erio d or amplitude

Acknowledgments JB wishes to acknowledge VEGA grant No supp ort the Royal

So cietyNATO Fellowship and to thank dr Zverko for making three observations

References

Adelman S J Astron Astrophys

Adelman S J Astron Astrophys Suppl

Adelman S J Brown B H Caliskan H Reese D F Adelman C J Astron

Astrophys Suppl

Aikman G C L P Dom Ap O

Bab co ck H W ApJS

Catalano F A Astron Astrophys Suppl

Catalano F A Renson P Astron Astrophys Suppl

ESA The Hipparcos Catalogue ESA SP

Harmanec P Horn J Juza K Astron Astrophys Suppl

Rakosch K D Fiedler W Astron Astrophys Suppl

Slettebak A Astrophys J

Winzer J E PhD Thesis University of Toronto

Zb oril M Buda j J IBVS No

COMMISSIONS AND OF THE IAU

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HU ISSN

THE SPECTRUM PERIOD AND PROPER MOTION OF V SCORPI I

J R THORSTENSEN

Dept of Physics and Astronomy Dartmouth College Wilder Lab oratory Hanover NH USA

email johnthorstensendartmouthedu

The dwarf nova V Sco was recently recovered by Kato et al Because its

identication was obscure for so long little is known ab out its outburst characteristics I

obtained sp ectra in June with the m Hiltner telescop e at MDM Observatory on

Kitt Peak details of the instrumentation reduction and analysis were essentially identical

to those in Thorstensen et al There are exp osures of  s each

Fig shows the mean sp ectrum and Table lists the sp ectral features detected He I I

is somewhat stronger than usual for a dwarf nova reminiscent of the Xray emitter

VZ Pyx Remillard et al Thorstensen and indeed Kato et al note

that V Sco is the likely counterpart of a ROSAT bright source The emission lines are

all doublep eaked with separation  km s in He I The dips in the central

cores of the emission lines app ear somewhat deep er than usual with the cores of HeI

extending down to the continuum in some exp osures The FWHM of the H emission is

A The continuum ux which is uncertain by  p ercent implies V

I measured radial velocities of H Table using a convolution metho d Schneider

and Young The convolution function used had p ositive and negative Gaussians

of A FWHM separated by A This emphasized the steep sides of the line prole

Fig shows the p erio d search residualgram Thorstensen et al It indicates a

p erio d near d though a daily cycle count alias at d is p ossible The Monte

d

Carlo test of Thorstensen Freed indicates that the p erio d is preferred at

the  p er cent condence level so the choice is fairly secure but not denitive Table

gives sinusoidal ts to the two aliases of the form

v t K sin t T

Fig shows the velocities folded on each of the two b est p erio ds

In addition to the sp ectra I acquired three second V band direct frames June

UT Fig shows a nding chart A t of this image to the USNO A catalogue

Monet et al and the Digital Sky Survey revealed signicant prop er motion since

the plate from which these were derived ep o ch The implied motion is

arcsec yr in p osition angle degrees with an uncertainty of approximately

arcsec yr

All dwarf novae with p erio ds similar to V Sco are SU UMa stars which show

sup eroutbursts and sup erhumps As the photometric prop erties of V Sco are explored

it is very likely that it to o will follow this pattern The substantial prop er motion and

bright apparent magnitude b oth suggest a relatively small distance

IBVS

Figure Mean sp ectrum of V Sco at minimum light

Figure Periodogram of the H velocities

IBVS

Figure Velocities folded on the b est p erio d upp er panel and on the secondb est alias lower

panel All p oints are shown twice for continuity

Figure Finding chart for V Sco derived from a June V band image Orientation and scale are indicated as is the p osition derived from a t to USNO A stars

IBVS

Table Sp ectral Features

a

Line EW A F



H 

HeI 

HeI I 

H 

HeI 

HeI 

HeI 

H 

HeI 

HeI 

a

Uncertain by  p er cent in erg cm s A

Table Radial Velocities of H

a b

HJD v HJD v HJD v HJD v

a b

Helio centric Julian date of midintegration minus Units of v are km s

Table Fits to H Velocities

a

P d km s K km s km s T

   

   

a

Helio centric Julian date minus

References

Kato T Haseda K Takamizawa K Kazarovets E V Samus N N IBVS

No

Monet D et al USNOSA US Naval Observatory Washington DC

Remillard R A Bradt H V Brissenden R J V Buckley D A H Schwartz D A

Silb er A Stro ozas B A and Touhy I R ApJ

Schneider D and Young P ApJ

Thorstensen J R Freed I W AJ

Thorstensen J R Patterson J Thomas G Shambrook A PASP

Thorstensen J R PASP

Thorstensen J R Taylor C J Kemp J PASP

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HU ISSN

CCD PHOTOMETRY OF THE ECLIPSING BINARY V CYGNI

1 2

ROGER DIETHELM MAREK WOLF

1

Astronomical Institute University of Basel CH Binningen Venusstrasse Switzerland

Email diethelmastrounibasch

2

Astronomical Institute Charles University Prague CZ Praha V Holesovickach Czech Republic

Email wolfmboxcesnetcz

The eclipsing binary V Cygni S Cyg GSC FL

h m s  0 00

J V mag was discovered photographically

max

in the eld of the star Cygni by Homeister in Sonneb erg Later Gessner

recognized the W UMatype and derived the rst light elements of low accuracy

Pri Min HJD  E

The CCD photometry of V Cyg presented here was carried out during eight nights

in August and November at the R Szafraniec Observatory Metzerlen Switzerland

with the cm SchmidtCassegrain telescop e and an unltered CCD camera SBIG ST

Additional measurements were done during the night of JD with the same

equipment The standard error of the measurements varies from mag to mag

The stars GSC V mag and GSC V mag on the

same frame as the variable served as comparison and check star resp ectively Figure

It is also remarkable that V Cyg is sup erimp osed on a faint galaxy  mag

whose nucleus lays slightly west of the variable This galaxy as well as V Cyg could

h m s  0 00

b e also identied with the source IRAS

J Altogether frames of this eld were obtained and analysed Table contains

three new ep o chs for minima N denotes the number of measurements used for the precise

determination of minimum time

Our CCD observations conrm the W UMatype of this eclipsing binary but we nd

a substantially shorter orbital p erio d of ab out days This p erio d also ts the

minima of Gessner b etter the corresp onding new cycle counts are given in Table

A recalculation of the light elements using the original times of minimum published by

Gessner and our new ep o chs gives the following result

Pri Min HJD  E

Our photo electric light curve was solved indep endently using a metho d of treating pho

tometric data describ ed by Mikulasek at al which is a weighted LSM iterative

IBVS

Figure Finding chart of V Cyg with the size of the eld  arcmin

Figure Comp osite light curve of V Cyg for the p erio d of days

IBVS

Table Times of minimum of V Cyg

HJD Ep o ch Ep o ch

Gessner this pap er

Error

Ep o ch N

days

published also in BBSAG Bul l No

pro cedure Using this metho d we derive the current light elements which could b e used

in the near future

Pri Min HJD  E

 

Figure shows the light curve folded with this p erio d The light amplitude for the primary

minimum according to our measurement is A  mag for the secondary

minimum we nd A  mag

The dierence of b oth derived p erio ds   day and a number of ep o chs elapsed

since the rst observations  gives value of days which is smaller than

the value of p erio d P or P Our newly determined ep o chs and the cycle count given in

Table is correct which might hints towards the existence of a p erio d change in the time

interval b etween Gessners data and ours Further observations of this eclipsing system

are necessary in order to establish a b etter value of the orbital p erio d andor its probable

changes Also an investigation on photographic plates could help solve this questions

Acknowledgements This work has b een supp orted in part by the Swiss National Sci

ence Foundation MW is very grateful for the use of the facilities and the hospitality at

the Astronomical Institute of University Basel in the August RD wishes to thank

the Emilia GuggenheimSchnurr Foundation for nancial supp ort

References

Gessner H Vero Sternwarte Sonneberg

Homeister C Astron Nachrichten

MikulasekZ HanzlD Horno ch K Contributions of Nicholas Copernicus Obser

vatory Brno

IBVS

ERRATUM

In the Table of IBVS No all sp ectral types MS should read M Therefore M

sp ectral type is assigned to XX CMa TU Car DL Cen BS Mon HW Mon W Mus

BO Pup ES Pup AD Vel and NSV The original manuscript was correct The

errors o ccurred when the OCR software was utilized With our ap ologies THE EDITORS

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PHOTOELECTRIC MINIMA OF SOME ECLIPSING SYSTEMS

T PRIBULLA D CHOCHOL S PARIMUCHA

Astronomical Institute of the Slovak Academy of Sciences SK TatranskaLomnica Slovakia

We present new minima times of RS CVn and W UMa systems taken from

August to July as a part of the program of the full lightcurve coverages

The U B V and R photo electric observations were taken at the Skalnate Pleso SP

and Stara Lesna SL observatories of the Astronomical Institute of the Slovak Academy

of Sciences In b oth cases the m Cassegrain telescop e equipp ed with a singlechannel

pulsecounting photo electric photometer was used For all observations a second inte

gration was used Data reduction the atmospheric extinction correction and transforma

tion to the standard system were carried out in the usual way

We have calculated the times of minima separately fo all lters using the Kwee and Van

Woerdens metho d parab ola t sliding integration metho d tracing pap er and center

of mass metho d which were describ ed in detail by Ghedini The computer co des

were kindly provided by Dr R Komzk The average times of the primary I

and secondary I I minima and their probable errors found by these metho ds are given in

Table

Table Times of minima of observed systems

HJD Min

System  Filter Obs

type

RT And II B SP

II V SP

II R SP

I U SL

I B SL

I V SL

II U SL

II B SL

II V SL

II B SP

II V SP

II R SP

I U SL

I B SL

I V SL

I B SP

I V SP

I R SP

II V SP

II R SP

II B SL

II V SL

IBVS

Table cont

HJD Min

System  Filter Obs

type

i Bo o I U SL

I B SL

I V SL

II U SL

II B SL

II V SL

II U SP

II B SP

II V SP

II R SP

I U SL

I B SL

I V SL

II U SL

II B SL

II V SL

II V SL

I V SL

II U SL

II B SL

II V SL

I B SP

I V SP

I R SP

II B SP

II V SP

II R SP

SV Cam I U SL

I B SL

I V SL

II U SL

II B SL

II V SL

I U SL

I B SL

I V SL

II V SP

II R SP

I B SP

I V SP

I R SP

I B SP

I V SP

I R SP

II B SP

II V SP

II R SP

I B SP

I V SP

I R SP

EG Cep I B SP

I V SP

I R SP

VW Cep II U SL

II B SL

IBVS

Table cont

HJD Min

System  Filter Obs

type

VW Cep II V SL

I U SL

I B SL

I V SL

II U SL

II B SL

II V SL

I U SL

I B SL

I V SL

I U SL

I B SL

I V SL

WY Cnc I U SL

I B SL

I V SL

AW UMa II U SL

II B SL

II V SL

I U SP

I B SP

I V SP

I R SP

W UMa I U SL

I B SL

I V SL

I U SL

I B SL

I V SL

II U SL

II B SL

II V SL

I U SP

I B SP

I V SP

I R SP

I U SL

I B SL

I V SL

I U SL

I B SL

I V SL

II B SL

II V SL

XY UMa I U SL

I B SL

I V SL

I B SP

I V SP

I R SP

II B SP

II V SP

II R SP

I B SP

I V SP

IBVS

Table cont

HJD Min

System  Filter Obs

type

XY UMa I R SP

II B SP

II V SP

II R SP

I B SP

I V SP

I R SP

I B SP

I V SP

I R SP

I U SL

I B SL

I V SL

I U SL

I B SL

I V SL

I B SP

I V SP

I B SP

I V SP

I R SP

II V SP

II R SP

I U SL

I B SL

I V SL

I U SL

I B SL

I V SL

II U SL

II B SL

II V SL

ER Vul II U SL

II B SL

II V SL

II U SL

II B SL

II V SL

II U SL

II B SL

II V SL

Acknowledgements This work was nancially supp orted by the VEGA grant

References

KomzkR private communication

Ghedini S Software for Photometric Astronomy WillmannBell Publ Comp Richmond

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RECENT LIGHT CURVES AND PERIOD STUDY OF

THE CONTACT BINARY W URSAE MAJORIS

JM DEPASQUALE JJ BOCHANSKI EF GUINAN

Astronomy Astrophysics Department Villanova University Villanova PA USA

W Ursae Ma joris HD is a wellknown FVFV eclipsing binary system and

is the prototype for W UMatype contact binaries A recent determination and discussion

of its prop erties is given by Linnell W UMa was recently observed at the Villanova

Observatory by J DePasquale C Henry I Nadalin and M Stump on the nights of

March and and April UT The observations were obtained

by using the same equipment and lters as describ ed in Morgan et al Over

new observations were recorded The comparison star was HD V

B V K and HD V B V K served as the check

star These were the same stars used previously at Villanova since and found to b e

constant in brightness The observations were reduced in the usual way with corrections

for dierential atmospheric extinction applied However b ecause of the angular proximity

of the comparison and variable stars the extinction corrections were very small Also

the UT times were converted to helio centric Julian Day number

The yellow and red observations were formed into light curves and are shown in Fig

ure In the gure the dierential magnitudes in the sense of variable minus comparison

star V C are plotted against orbital phase The phases were computed using up dated

light elements so that recent primary minima o ccur at phase

T min I HJD  E

As can b e seen in the gure the light curves are well dened and show the characteristic

continuous light variations that are typical for W UMatype binaries The light varia

tions arise from the mutual eclipses of the comp onent stars as well as from chiey tidal

distortion and reection eects The light curves are similar but not identical to the

ones rep orted earlier by Morgan et al using the same equipment and lters As

is usually the case for W UMa the light curves show small asymmetries that change

with time The maximum at phase is ab out mag fainter than the maximum

at phase in the y bandpass and ab out mag fainter in the red bandpass As

shown in Fig there is also a noticeable distortion in the light curve near the b ottom of

primary eclipse These asymmetries and photometric anomalies most likely arise from the

presence of starsp ots on one or b oth stars of the system see eg Guinan Bradstreet

W UMa and typically most W UMatype stars with co ol comp onents display

the manifestations of strong magneticdynamo activity such as enhanced chromospheric emissions strong coronal Xray emission and photometric anomalies in their light curves

IBVS

Figure Figure

IBVS

pro duced by large starsp ots see eg Guinan Gimenez Preliminary analyses of

the MarchApril light curves indicate the presence of at least two sp ot regions on

the stars One extended sp otted region is most visible near phase and pro duces

the small depression in the light curves seen during the quadrature near phase

Several primary and secondary minima were observed during Times of minimum

light were determined from least squares parab olic ts to the eclipse data Also timing

determinations were made by reecting the ingress and egress branches of the eclipses to

check the least squares ts Both metho ds yielded consistent results when the observations

in the lower half of the eclipses were used in the analyses Times of minimum light were

indep endently determined for the yellow and red data but no systematic dierences were

found However the yellow data had less scatter and yielded somewhat higher precisions

to the timings The new minima are given in Table Additional eclipse timings were

obtained from unpublished observations made at Villanova during These

additional determinations are listed in Table as well

Table Times of Primary and Secondary Eclipses of W UMa

Filter Type JD Hel Observer

r I S Margheim

bn I

r I S West

bn I

r II

bn II

y II R Mittal

r II

y II R Slevinsky

r II

y I P Dituro

r I

y I J DePasquale

r I

y II I Nadalin

r II

y I

r I

y II J DePasquale

r II

y I M Stump

r I

r nm bn nm y nm

Morgan et al have carried out a p erio d study of W UMa from observations

collected at Villanova from to and found that the p erio d has b een relatively

constant during that interval In Figure we extend this study to by combining the

minima given here with those already published by Morgan et al In the gure

the O C values are plotted against the number of cycles elapsed E O C values were

calculated with the ephemeris used previously by Morgan et al Linear solid line

and parab olic dotted curve least squares ts were made to the data but as shown in

IBVS

the gure there is little dierence b etween them Thus for this interval of time we adopt

a linear t and the mean p erio d during this time interval is P d

(19821999)

This is the same value found by Morgan et al However W UMa has a long history

of complicated changes in apparent p erio d over time see eg Hamzaoglu et al

and Morgan et al and that the relatively constant p erio d found over the last

years is probably transitory However the light elements given ab ove may b e used to

predict eclipses over the next few years

A closer examination of the Figure also reveals p ossible small  d systematic

residuals of the O C values from the linear or quadratic ephemeredes These shortterm

variations could arise from asymmetries in the light curve caused by the presence of dark

starsp ots that skew the shap e of the minima and pro duce apparent shifts in the measured

mideclipse times The residuals also could b e pro duced from dynamical eects either

from small changes in the orbital p erio d or from the lighttime eect of a third b o dy

However if a third b o dy were present then the resulting residuals would b e p erio dic in

nature This do es not app ear to b e the case from the present data As p ointed out by

Morgan et al the present p erio d is ab out sec shorter than previous values The

apparent decrease of the p erio d with time could arise from angular momentum loss from

magnetic braking or could b e due to mass transfer b etween the comp onents

Additional photo electric photometry of W UMa is planned at Villanova University

Observatory This research is supp orted in part from a NSFRUI grant AST to

Villanova University which we gratefully acknowledge For this research we utilized the

SIMBAD database op erated by CDS Strasb ourg France

References

Guinan EF Bradstret DH in Formation and Evolution of Low Mass Stars

eds AK Dupree MT Lago Kluwer Academic Publ Dordrecht p

Guinan EF Gimenez A in The Realm of Interacting Binary Stars eds J

Sahade GE McCluskey and Y Kondo Kluwer Academic Publ Dordrecht p

HamzaogluE Keskin V Eker T IBVS No

Linnell AP ApJ

Morgan et al IBVS No

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UBV OBSERVATIONS OF THE MASS EXCHANGING

SOLARTYPE BINARY BE CEPHEI

1;3 1 1 1 1

RONALD G SAMEC NW GOTHARD BC PARKER TW SAVAGE SD ANDERSON

2;3

DANNY R FAULKNER

1

Department of Physics Bob Jones University Greenville SC USA rsamecb juedu

2

University of South CarolinaLancaster Lancaster SC USA faulknergwmscedu

3

Visiting Astronomer Lowell Observatory

Recently we b egan an observation program aimed at obtaining precision multiband

d d

photometry of short p erio d solar type binaries in the to p erio d range In this

group we exp ected to nd some eclipsing binaries in a very near a state of contact

with one comp onent exp eriencing Ro chelobe overow Systems with unambiguous EB

light curves and complicating asymmetries were targeted BE Cephei SVS Cep

h m s  0 00

GSC RA DEC is such a candidate

Figure Finding chart from The Palomar Sky Survey of BE Cephei V the comparison star C and the check star K

IBVS

Figure O C residuals for all available timings of minimum light as calculated from Equation

Figure U B V light curves and U B B V color curves for BE Cephei as standard magnitude dierences variable minus comparison star

IBVS

Table Ep o chs of Minimum Light BE Cep

JD Hel

Cycles O C O C Source

KL

PO

PO

PO

PO

PO

PO

BE

BE

Sources KL Kaluzny

BE BBSAG E Blatte

PO Present Observations

BE Cep was discovered by Florija whose light curve is of EBtype with an

dierence of eclipse depths of mag He calculated the following light elements

JD Hel Min I  E

Homan to ok B V photo electric observations and archived them Kaluzny

used the observations to determine two timings of minimum light and to calculate a

B curve solution from phasebinned averages He p erformed a grid of solutions with

nonphysical alb edo es to and gravity darkening xed at to accommo date the light

curve distortions Subsequent times of minimum light have b een published by Romano

Ashbrook Borovicka Kolarova and in the BBSAG

issues and all by Kurt Lo cher and the BBSAG and

by Ernst Blatter with CCD

Our present UBV observations were taken with the Lowell m reecting tele

scop e on the nights of July RGS and DRF and September and

DRF with a thermo electrically blueenhanced S catho de PMT Ab out

observations were taken at each lter The comparison GSC RA

h m s  0 00

DEC and check star GSC RA

h m s  0 00

DEC are shown as C and K in Figure along with the

variable V The V C magnitudes averaged mags and mags in B V and

U B resp ectively Preliminary photometric transformations yield B V which

corresp onds to a G sp ectral type for the primary comp onent The magnitude range is

in V

Six mean ep o chs of minimum light were determined from the observations made during

three primary and three secondary eclipses by our undergraduate researchers using the

bisection of chords technique These precision ep o chs of minimum light are given in

Table along with their standard errors in parentheses Linear and quadratic ephemerides

were calculated using the available ep o chs of minimum light

JD Hel Min I  E

JD Hel Min I  E   E

Equations and were used to calculate the O C and O C residuals resp ectively

in Table The linear residuals are shown in Figure

IBVS

The UBV light curves and the B V and U B color curves of the variable are shown

as Figure as dierential standard magnitudes V C versus phase The probable

error of a single observation was and mmag in U B and V resp ectively A

near contact solution with a stream impact sp ot and co ol sp ot has b een computed using

the Wilson Co de Wilson Wilson Devinney The nal parameters

include T T K m m and lloutfactor The impact

sp ot parameters are colatitude longitude Sp ot Radius TFactor

We wish to thank Lowell Observatory for their allo cation of observing time for the travel

supp ort from the University of South Carolina and Bob Jones University particularly

Dr James Roach physics chair for allowing us to include binary star analysis as a part

of our regular department curriculum

This research was partially supp orted by a grant from NASA administered by the

American Astronomical So ciety

References

Ashbrook J AJ

Ashbrook J AJ

Borovicka J BRNO

Florija N Per Zvezdy

Homan M Veroder Astron Inst Bonn c

Kaluzny J PASP

Kolarova H BRNO

Romano R Padua Pub

Wilson R E ApJ

Wilson R E PASP

Wilson R E Devinney E J ApJ

COMMISSIONS AND OF THE IAU

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COMMENTS ON THE LIGHT CURVE OF V Her

RAYMOND H BLOOMER JR ISSA R NGWELE

King College King College Road Bristol TN USA

email rhbloomeking edu ingwelekingedu



Kaiser rep orted on the eclipsing system V Her SAO BD

GSC DHK Kaiser et al later published a p erio d and V light

m

curve that showed Beta Lyraelike variations for this V star During June

we recorded V and R images with a liquid nitrogenco oled Photometrics CCD

attached to the Air Force Academys m reector Images were bias subtracted and

at elded and magnitudes of the variable and several nearby stars were extracted using

m

IRAF routines The check star GSC V and the comparison star

m 0

GSC V were within the eld We found the dierences in

m

magnitude b etween these two stars in V light had a standard deviation of and the

m

dierences in R had a standard deviation of indicating their reasonable stability

The check star may b e slightly variable however

Using the metho d of KweeVan Woerden we established one new time of secondary

minimum light

Min I I HJD 

Using a linear least squares tting routine and weighting all the times given by Kaiser

and the current pap er by the inverse square of their standard errors estimating the

d

standard error of the old photographic times as we found new light elements hardly

signicantly dierent from Kaisers

d

Min I HJD  E

 

The O C s indicate no denite p erio d changes over the ep o chs used for this

p erio d study

The V and R magnitudes were converted to intensities and were then formed into

normal p oints by averaging over phase bins wide

To achieve a preliminary solution the intensity normal p onts were tted with a the

oretical curve using the program Binary Maker by David Bradstreet We assumed a

temp erature of K for the F primary star Figure shows the t for the V light



curve when the inclination is set at the secondary star has a temp erature of K

and the near contact conguration suggested by Kaiser We concur with Kaiser that

m

the maximum at phase is slightly brighter than that at by approximately

There was to o little R data to determine a solution though is not inconsistent with that

m

given here for V The depths of the eclipses relative to the brighter maximum are

IBVS

m m m

and in V and approximately and in R light We hop e to acquire more

photometric data esp ecially in the R so that we can nd a more denitive solution for the system

1.00

0.90

0.80

0.70 Flux 0.60

0.50

0.40

0.00 0.25 0.50

Phase

Figure V Intensity Light Curve and Binary Maker Fit

Acknowlegements We thank the Air Force Academy for generous telescop e time and

Drs Jack Wetterer and Shane Burns for their able assistance We thank the Appalachian

College Asso ciation for a StudentFaculty Research Grant that made this work p ossible

This research made use of the SIMBAD database op erated by the CDS Strasb ourg

France

References

Bradstreet DH Binary Maker Light Curve Synthesis Program Contact Soft

ware Norristown PA USA

Kaiser DH Inform Bul l Var Stars No

Kaiser DH Lub cke G Williams DB Inform Bul l Var Stars No

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ABSOLUTE PROPERTIES OF ZZ URSAE MAJORIS

CLAUD H SANDBERG LACY AND JEFFREY A SABBY

Department of Physics University of Arkansas Fayetteville AR USA

Radial velocities have b een measured on sp ectrograms obtained with the Kitt Peak

National Observatory coudefeed CCD sp ectrometer b etween May and May A

typical sp ectrogram is shown in Fig Radial velocities were obtained by crosscorrelation

with suitably broadened sp ectra of the radial velocity standard Vir RV kms

Mayor Maurice The radial velocities are listed in Table

We have adopted an eclipse ephemeris based on the dates of minima of Mallama

and Hanzl

d

Min I n JD

 

We have tted a circular sp ectroscopic orbit given in Table The tted orbit is displayed

in Fig The residuals from b oth the primary and secondary orbits were kms We

have combined our sp ectroscopic orbits with the photometric orbit of Clement et al

the results are shown in Table

Table Helio centric radial velocities of ZZ UMa

RV kms RV kms

HJD HJD

Primary Secondary Primary Secondary

IBVS

Figure Typical sp ectrogram of ZZ UMa near nm Lines of the secondary comp onent are

displaced to the left blueward at the phase shown

Figure Sp ectroscopic orbits of the comp onents of ZZ UMa The primary hotter and more massive

comp onent is represented by op en circles the secondary by lled circles

IBVS

Figure The comp onents of ZZ UMa solid circles with error bars in the massradius plane Op en

circles corresp ond to accuratelyknown comp onents of eclipsing binaries The curve is the theoretical

ZAMS of Schaller et al

Figure The comp onents of ZZ UMa in the massluminosity plane The symbols are the same as in Fig

IBVS

Table Absolute prop erties of ZZ UMa

Parameter Symbol Primary Secondary

Relative radius r  

Orbital inclination degrees i 

Visual central surface brightness J 

v

Intrinsic color index mag b y  

Temperature K T  

Radial velocity semiamp kms K  

Centerofmass radial vel kms  

Observed rotational vel kms v sin i  

Mass solar units M  

Radius solar units R  

Surface gravity cms log g  

Synchronous rotational vel kms v sin i  

Luminosity solar units log L  

Absolute visual mag M  

v

Distance p c 

The results are displayed in Figs Our results dier from those of Clement et

al due to improved accuracy of the sp ectroscopic orbits and due to a signicantly

redder adopted color index for the secondary comp onent Our color index is based on the

visual central surface brightness of the secondary which is a parameter of the photometric

orbit through the equation in Lacy et al F log J Poppers cali

v c

bration his Table was used to convert from surface brightness parameters into eective

temp eratures The primary comp onent parameters are well tted by theoretical mo dels

such as those of Schaller et al or Claret Gimenez for solar comp osition

at an age of ab out  yr but the secondary comp onent can not b e well tted by

any of the current mo dels b ecause it is co oler than predicted by the mo dels The origin

of this discrepancy is unknown

References

Claret A Gimenez A AAS

Clement R Garcia M Reglero V Suso J Fabregat J AAS

Hanzl D IBVS No

Lacy CH Frueh ML Turner AE AJ

Mallama AD ApJS

Mayor M Maurice E in Stellar Radial Velocities ed AG Davis Philip

David W Latham Davis Press p

Popper DM ARAA

Schaller G Schaerer D Meynet G Maeder A AAS

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HU ISSN

NSV AN RR LYRAE TYPE STAR IN LIBRA

1 1 2

P MERCHANBENITEZ M JURADOVARGAS F SANCHEZBAJO

1

Departamento de Fsica Facultad de Ciencias Universidad de Extremadura Avda de Elvas sn

Bada joz Spain email p edromerunexes mjvunexes

2

Departamento de Electronicae IngenieraElectromecanicaEscuela de IngenierasIndustriales Universidad

de Extremadura Avda de Elvas sn Bada joz Spain email fsanba jounexes

Name of the ob ject

NSV CSV

Equatorial co ordinates Equinox

h m s  0 00

RA DEC

Observatory and telescop e

Observatorio del Departamento de Fsicade la Universidad de Extremadura m

f Newtonian Reector

Detector Starlight Xpress CCD Camera based in the chip SONY

ICXBL  mm  pixels

Filters V KronCousins system

Comparison stars GSC

Check stars GSC

Transformed to a standard system No

Availability of the data

Up on request

Type of variability RR Lyr

Remarks

The results of the observations carried out show that NSV seems to b e an

RR Lyrae star with a p erio d close to hours The star shows an almost symmetric

light curve M mP and a magnitude amplitude in the V band

From the timing of four minima see Table obtained according to the KweeVan

Woerden metho d the following ephemeris for the maximum was derived

d

Max HJD  E

 

IBVS

Table

HJD Ep o ch O C

Acknowledgements

This research was supp orted by the Consejerade Educaciony Juventud Junta de

Extremadura and Fondo So cial Europ eo under pro ject IPRA

Figure The V light curve obtained for NSV Figure Identication chart of NSV C

Magnitude dierences variable minus Comparison star Ch Check star North is

comparison are plotted versus phase where the on the top

phases are computed using the ephemeris calcu

lated in this work

References

Kukarkin et al New Catalogue of Susp ected Variable Stars Moscow

Kwee KK Van Woerden H BAN

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CCD PHOTOMETRY OF THE

FEBRUARY OUTBURST OF CI Gem

1 2

T KATO P SCHMEER

1

Dept of Astronomy Kyoto University Kyoto Japan email tkatokusastrokyotouacjp

2

Bischmisheim Am Probstbaum D Saarbr ucken Germany email extpascrzunisbde

CI Gem is a variable star discovered by Homeister He prop osed the

novalike or dwarf novatype classication based on the single outburst Duerb eck

prop osed the p ossible quiescent counterpart and suggested the dwarf nova nature based

on the small outburst amplitude Wenzel examined Sonneb erg plates and found

three additional outbursts b etween and From the existence of long and short

outbursts Wenzel suggested the SU UMatype classication

An additional outburst of CI Gem was detected by P Schmeer on an unltered

CCD image taken on February UT the discussion on the outburst detection is

also given in Schmeer and Duerb eck He rep orted the ob ject as magnitude

Schmeer rep orted the incorrect quiescent identication by Duerb eck the

precise co ordinates are given by Schmeer and Duerb eck Schmeer rep orted

nothing down to magnitude was visible on the POSS blue print at this lo cation

.04

CI Gem

.03

.02

Relative flux .01

0

-.01 29 29.5 30 30.5 31 31.5 32 32.5 33

HJD - 2451200

Figure Overall light curve of CI Gem

IBVS

Table Nightly averaged magnitudes of CI Gem

a b c d

midHJD mag error N

a

HJD

b

Magnitude relative to GSC

c

Standard error of nightly average

d

Number of frames

The observations were done on ve nights b etween February and using an

unltered ST camera attached to the Meade cm SchmidtCassegrain telescop e The

exp osure time was s The images were darksubtracted atelded and analyzed using

TM

the Java based PSF photometry package developed by the author TK The lo cation

of the PSF center was adjusted using Schmeers astrometry The ux of the variable

was measured relative to GSC USNO r magnitude whose constancy was

conrmed by comparison with GSC USNO r magnitude

Figure illustrates the overall light curve of the present observation The uxes are

given relative to GSC Table summarizes the nightly averaged magnitudes

As seen in Table and Figure CI Gem was already fading rather rapidly By

adopting the USNO r magnitude of the comparison CI Gem was estimated to b e 

on February and  on February The last part of the light curve however

may have b een aected by the nearby star The average decline rate mag d

of the initial part of the observation precludes the sup eroutburst However the decline

rate seems to b e a little slower than those of normal outbursts of SU UMa stars usually

exceeding mag d Period analysis of February and observations spanning

and hr resp ectively o ccasionally interrupted by gaps could not yield p ositive

p erio dicities b etween and d to a limit of mag Although this negative result

do es not preclude a normal outburst of an SU UMa star the present observation seems

to suggest a longer orbital p erio d system p ossibly an SS Cygtype dwarf nova

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture and Sp orts

References

Duerb eck H W Space Sci Rev

Homeister C Astron Nachr

Homeister C Vero Sternwarte Sonneberg

Schmeer P VSNET alert circulation No also available from

httpwwwkusastrokyotouacjpvsnetMailvsnetalertmsghtml

Schmeer P Duerb eck H W IBVS No

Wenzel W IBVS No

COMMISSIONS AND OF THE IAU

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THE FEBRUARY OUTBURST OF THE

DWARF NOVA CI Gem

1 2

PATRICK SCHMEER AND HILMAR W DUERBECK

1

Am Probstbaum Saarbr ucken Germany email extpascrzunisbde

2

WEOBSS University of Brussels VUB Pleinlaan Brussels Belgium email hduerb ecvubacb e

CI Gem S is a p o orly known cataclysmic variable It was discovered by Homeis

ter on Sonneb erg plates as a dwarf nova or novalike star it reached a maximum of

m

m on Jan declined by ab out in the subsequent days and dropp ed

pg

b elow the plate limit after days The light curve is shown in Ahnert et al and

Wenzel A handdrawn nding chart was published by Homeister On

this basis Duerb eck tentatively identied CI Gem at its minimum stage with a

m

fairly blue star of This star is listed as in the USNOA catalog

CDS VizieR service

Wenzel rep orted three additional outbursts on Octob er m

pg

February m and December m

pg pg

A new outburst was found by one of us PS on an unltered CCD frame taken

February UT by Mark Parker with the UC Santa Barbara Celestron telescop e

On a unltered frame taken February UT with the University of Iowa m IRO

rob otic telescop e the ob ject was still b elow or at R  Ap erture photometry of

the discovery image yields R  using a lo cal sequence by Duerb eck in preparation

On February UT Pepe Vilchez and Peter Sorensen used the wide eld camera

at the prime fo cus of the m Isaac Newton telescop e INT They obtained one B and

two R frames which show the ob ject at B R Fig Additional images

from IRO yield R  and on February and UT resp ectively

According to Kato and Schmeer see also

httpwwwkusastrokyotouacjpvsnetLCsindexgemcihtml

m

CI Gem was at V on February UT and dropp ed by in three days

Its p osition was determined on the INTframes using seven nearby stars selected from

the USNOA catalog with the aid of the MIDASASTROMET package

h m s  0 00

RA Decl equinox J

00

It lies ab out south of

Archival CCD frames of the eld taken January with the ESODanish m

telescop e at La Silla clearly show a fairly red ob ject at the exact place of CI Gem with

V B V V R Fig In B the ob ject is at the limit of visibility

m

and the error in the colour index may amount to several

IBVS

Figure The eld of CI Gem in and in taken in the R band with the ESODanish m

telescop e and the Isaac Newton m telescop e resp ectively North is up and west to the right The

00 00

eld is ab out  The outburst image of coincides with a faint starlike ob ject in the centre

of the image Some nonstellar ob jects are found in its vicinity

IBVS

The galactic extinction was estimated using the routine EXTINCT by Hakkila et

al It reaches a maximum value of A  at kp c Thus the red

V

colour of CI Gem cannot b e due to interstellar reddening Several neighbouring ob jects

are clearly galaxies also an indication of low reddening in this direction The starlike

app earance of the ob ject at minimum makes the identication quite certain

The eruption was a bright outburst which lasted more than days The

outburst listed by Wenzel was also bright but of unknown duration while the out

burst was denitively fainter and shorter days The and outbursts were

also faint but to o fragmentarily observed to p ermit any conclusions on their character

We are reluctant to classify this ob ject as an SU UMatype dwarf nova as was done

by Wenzel Kato and Schmeer analyzed photometry carried out during the

recent outburst and found no p erio dicities b elow hours A more imp ortant criterion is

the colour At minimum SU UMatype systems tend to have B V values around

while SS Cygtype systems usually app ear redder with B V values around Bruch

and Engel SS Cygtype systems may also show long and short outbursts eg SS

m

Cyg itself has preferred outburst lengths of and days amplitudes of as

well as outburst intervals of several days Warner Vogt established a

statistical relation b etween orbital p erio d and B V colour at minimum the colour of

CI Gem indicates a p erio d of hours

The outburst characteristics of CI Gem in combination with its red colour at minimum

favour its classication as SS Cygtype dwarf nova Only timeresolved photometry during

a long outburst can establish the subtype b eyond doubt

Acknowledgment We thank Mark Parker UCSB Rob ert Mutel and his students

University of Iowa Pepe Vilchez IAC and Peter Sorensen ING for carrying out the

observations

References

Ahnert P Homeister C Rohlfs E van der Voorde A VeroSternw Sonneb erg

Bruch A Engel A Astr Astrophys Suppl

Duerb eck HW A Reference Catalogue and Atlas of Galactic Novae Dordrecht

Reidel Space Sci Rev

Hakkila J Myers JM Stidham BJ Hartmann DH Astr J

Homeister C Mitt VeranderlSterne No

Kato T Schmeer P Inf Bull Var Stars No

Vogt N habilitation thesis Bo chum University p

Warner B Cataclysmic Variable Stars Cambridge Cambridge University Press

Wenzel W Inf Bull Var Stars No

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

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THE FEBRUARY SUPEROUTBURST OF THE

SU UMaTYPE DWARF NOVA CG CMa

HILMAR W DUERBECK PATRICK SCHMEER JOHAN H KNAPEN DON POLLACCO

1

WEOBSS University of Brussels VUB Pleinlaan Brussels Belgium email hduerb ecvubacb e

2

Am Probstbaum Saarbr ucken Germany email extpascrzunisbde

3

University of Hertfordshire Department of Physical Sciences Hateld Herts AL AB UK

email knap enstarhertsacuk

4

Isaac Newton Group Santa Cruz de La Palma Tenerife Spain email dlpingiaces

CG CMa is a p o orly known cataclysmic variable It was discovered by C Verlooy on

FranklinAdams plates taken in January Maximum light m was observed

pg

m

on January the ob ject had b een b elow the plate limit of four days b efore

m

It declined in ab out days and subsequently fell b elow the plate limit Van Ho of

published a discovery note with the light curve and a handdrawn nding chart

He classied it as apparently a faint nova PayneGaposchkin noted the unusual

p osition of this nova near the galactic anticentre at a large galacto centric distance if

a typical nova luminosity is assumed and commented CG CMa might prove to b e a U

Gem star or a recurrent nova

On the basis of the nding chart and an additional Harvard photograph of quite in

sucient plate scale Duerb eck tentatively identied CG CMa at its minimum

stage with a star of m This star is listed as in the USNOA

pg

catalog CDS VizieR service with magnitudes B R Because of the ap

parently small outburst amplitude dwarf nova variability was susp ected A sp ectroscopic

investigation by Zwitter and Munari yielded an A type sp ectrum and the authors

susp ected white dwarf characteristics

The discovery of a new outburst on February UT by R Stubbings

lead us to reconsider the case B V R and I frames of the eld were obtained by JHK

at the Cassegrain fo cus of the m Jacobus Kapteyn telescop e at La Palma on

March UT They show the ob ject as a close companion to Using

a lo cal sequence by Duerb eck in preparation CG CMa yields the following magnitude

and colours at this late stage of the outburst V B V V R Its

p osition and that of the USNO star were determined using sixteen nearby stars selected

from the USNOA catalog with the aid of the MIDASASTROMET package

h m s  0 00

CG CMa RA Decl equinox J

h m s  0 00

RA Decl equinox J

00

CG CMa lies ab out east of The co ordinates of b oth stars are in very

go o d agreement with those measured by Henden

IBVS

Figure The eld of CG CMa in R band at minimum and in I band at outburst

North is on top and west to the right The dwarf nova is the eastern comp onent of the close double star

00 00

in the centre of the image The eld size is ab out  At minimum no counterpart is seen down

m

to R

IBVS

CG CMa was b elow V on February UT it reached V

m

on February and had fallen by around March according to data

published in VSNET

httpwwwkusastrokyotouacjpvsnetLCsindexcmacghtml

m

Thus the decline in days is faster than that of The brightness declines must

always b e treated with caution b ecause they are based on the combined light of b oth

stars

Archival CCD frames of the eld taken January with the ESODanish m

telescop e at La Silla by HD show no trace of CG CMa at minimum

yields V B V V R The and frames are shown in

Fig Using IRAFDAOPHOT the prole of the companion star was subtracted on the

frame but the residual image also do es not show a trace of the cataclysmic variable

m m

We estimate a bright limit of ab out in V and R and ab out in B for CG CMa at minimum

8000 Bowen

7000

6000 flux He I

5000 He I

4000 400 500 600 700

wavelength (nm)

Figure The sp ectrum of CG CMa on February UT in the early stages of the outburst

A few sp ectral features are marked

A sp ectrum of CG CMa was obtained by DP with the m Isaac Newton telescop e

on February UT in the early stages of the outburst with an exp osure time

of sec Fig Sup erimp osed on a strong continuum which rises towards shorter

wavelengths H app ears as a strong emission line surrounded by a broad absorption

trough whose full width corresp onds to kms H also app ears as an emission

embedded in a broad trough full width kms but it is so weak that it hardly

reaches the continuum level Higher Balmer lines may show a similar structure The

Bowen complex He I I C I I IN I I I app ears as a strong emission and lines of

IBVS

He I at and nm are also in emission The full width at half maximum of the

emission lines H H and He I I is ab out kms The sp ectrum is quite typical

of SU UMatype dwarf novae at sup eroutburst see eg the descriptions of RZ Leo and

HV Vir Cristiani et al della Valle et al

The brightness at maximum of GC CMa is ab out B if one takes van Ho of s

maximum observation m at face value and estimates B from Stubbings

pg

visual observations by applying the B V colour index observed later in the outburst

m

Thus the amplitude is larger than Brightness mo dulations with a sup erhump p erio d

of days were observed in the last days of February Kato et al These

facts together with the sp ectral app earance and the apparently long recurrence time

make CG CMa a certain member of the SU UMa group of dwarf novae p ossibly of WZ

m

Sge subtype Such ob jects have absolute visual magnitudes at minimum b etween and

m m

and in extreme cases may b e as faint as Warner The galactic extinction

as estimated using the routine EXTINCT by Hakkila et al is very low A

V

m

at kp c Assuming a value for the absolute magnitude a lower limit of ab out

p c can b e set to the distance of CG CMa

References

Cristiani S Duerb eck HW Seitter WC IAU Circ No

della Valle M Duerb eck HW Motch C IAU Circ No

Duerb eck HW A Reference Catalogue and Atlas of Galactic Novae Dordrecht

Reidel Space Sci Rev

Hakkila J Myers JM Stidham BJ Hartmann DH Astr J

Henden AA VSNETchat

Kato T Matsumoto K Stubbings R Inf Bull Var Stars No

PayneGaposchkin C in Novae and Related Stars ed M Friedjung Dordrecht

Reidel p

Stubbings R VSNETalert

van Ho of A Publ Lab Astronomie et Geodesie de l Universite de Louvain

No p

Warner B Cataclysmic Variable Stars Cambridge Cambridge University Press

Zwitter T Munari U Astr Astrophys Suppl

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CCD PHOTOMETRY OF THE OUTBURST OF CG CMa

1 1 2

T KATO K MATSUMOTO R STUBBINGS

1

Dept of Astronomy Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp katsurakusastrokyotouacjp

2

Greenland Drive Drouin Victoria Australia email stubb oqedsystemscomau

CG CMa was discovered by Verlooy on FranklinAdams plates taken in Accord

ing to Duerb eck the maximum was reached on January The ob ject had

b een considered as a p ossible classical nova one of most distant in our Galaxy However

Duerb eck identied the p ossible quiescent counterpart and discussed the p ossi

bility of a dwarf nova based on the outburst amplitude The cataclysmic classication

however b ecame less likely when Zwitter and Munari to ok the sp ectrum of the

suggested quiescent counterpart yielding shallow absorption lines resembling those of an

isolated white dwarf

The ma jor breakthrough in understanding the nature of this ob ject was brought by

visual monitoring by R Stubbings His second historical outburst detection on

February Stubbings provided a unique opp ortunity in unveiling the enigmatic

ob ject The rep orted magnitude was m on February UT On February

v

the ob ject was invisible b elow mag

The CCD observations were done using an unltered ST camera attached to the

Meade cm SchmidtCassegrain telescop e The exp osure time was s The images

TM

were darksubtracted atelded and analyzed using the Java based PSF photometry

package developed by one of the authors TK

So on after the initial observation we realized the outbursting ob ject is slightly o

set from the suggested quiescent counterpart Using eight GSC stars mean residual

00 h m s  0 00

we obtained the co ordinates of J Using the

December image taken at Ouda Station we yielded the co ordinates of the prop osed qui

h m s  0 00

escent counterparts as J on the same reference frame

00

The latter co ordinates b eing within of the USNO A p osition it is now evident

the outbursting ob ject is dierent from Duerb ecks candidate The nding was

conrmed by Henden and Duerb eck et al who actually resolved the two

comp onents We in the following analysis consistently used the newly obtained co or

dinates of the outbursting ob ject for lo cating the ap erture and PSF but b ecause of the

small separation of two comp onents b eing always smaller than the seeing size the ob

tained uxes should b e considered as the combined light At the brightest ep o ch of CG

CMa the contribution of the fainter companion was estimated as The ux of the

variable was measured relative to GSC V B V Sumner

IBVS

Table Nightly averaged magnitudes of CG CMa

a a b c d

JD start JD end mean mag error N

a

JD

b

Magnitude relative to GSC

c

Standard error of nightly average

d Number of frames

3 CG CMa

4 Relative magnitude 5

6

30 35 40 45 50 55 60

JD - 2451200

Figure Overall light curve of CG CMa

IBVS

and Henden whose constancy was conrmed by comparison with GSC

Table summarizes the observations

Figure illustrates the overall light curve of the outburst of CG CMa We consider

the JD p oint as the representative brightness of the companion quiescent

brightness The star initially declined at a rate of mag d for seven days then

the decline b ecame slower Even after days after the outburst maximum the ob ject

remained signicantly brighter than quiescence The outburst thus lasted more than

days The overall light curve strongly resembles those of WZ Sgetype dwarf novae eg

AL Com Nogami et al A p ossible fading although the error was large due to the

weather at JD day past maximum may corresp ond to a dip observed in AL Com Nogami et al

1.02

1.01 CG CMa

1

.99 theta

.98

.97 P=0.0636

.96

13 14 15 16 17 18

Frequency (1/d)

Figure Period analysis of CG CMa

We searched for sup erhump mo dulations in the timeseries data There was no marked

oscillation for the rst two nights but the wave emerged on February JD

The Phase Disp ersion Minimization PDM Stellingwerf analysis was applied for

the February data after removing the steadily declining trend The resultant theta

diagram is shown in Figure The b est p erio d was  d

The sup erhump prole folded by this p erio d is shown in Figure The prole is that

of typical welldeveloped sup erhump The full amplitude is mag

From the typical app earance of sup erhumps we conclude CG CMa is a short p erio d

SU UMatype dwarf nova rather than a classical nova The long duration and the prole

of the outburst particularly suggest a WZ Sgetype classication which rarely show out

bursts The inferred large outburst amplitude which is a characteristic of WZ Sgetype

dwarf novae do es not contradict with the astrometric implications Henden

IBVS

-.15

-.1

-.05

0

Relative magnitude Relative .05

.1

.15 -.4 -.2 0 .2 .4 .6 .8 1 1.2 1.4

Superhump phase

Figure Sup erhump prole of CG CMa

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture and Sp orts TK Part of this

work is supp orted by a Research Fellowship of the Japan So ciety for the Promotion of

Science for Young Scientists KM

References

Duerb eck H W Space Sci Rev

Duerb eck H W Schmeer P Knap en J H Pollacco D IBVS No

Henden A VSNET chat circulation No also available from

httpwwwkusastrokyotouacjpvsnetMailvsnetchatmsghtml

Nogami D Kato T Baba H Matsumoto K Arimoto J Tanabe K Ishikawa K

ApJ

Stubbings R VSNET alert circulation No also available from

httpwwwkusastrokyotouacjpvsnetMailvsnetalertmsghtml

Stellingwerf R F ApJ

Sumner B Henden A VSNET chat circulation No also available from

httpwwwkusastrokyotouacjpvsnetMailvsnetchatmsghtml

Zwitter T Munari U Astron Astrophys Suppl

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

September

HU ISSN

PRECISE COORDINATES OF VARIABLE STARS

T KATO

Dept of Astronomy Faculty of Science Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp

This rep ort contains accurate p ositions for variable stars discovered by Homeister

The variable stars listed in Table were identied against computer plots of GSC

and USNO A catalogs The color information and IRAS PSC identication were also

examined in identifying red variables The source of identication in column source

GSC GSC GSC mean average of GSC multiple entries USNO USNO

A USNO mean average of USNOA multiple entries

PY Tel S given as Mtype in GCVS Homeister classied as shortp erio d

p ossibly RR Lyrtype The USNO color is not red

V Sgr S brighter one of two candidate stars

Detailed information of identications other catalog identications are available from

the VSNET archive vsnet

httpwwwkusastrokyotouacjpvsnetMailvsnetmsghtml

httpwwwkusastrokyotouacjpvsnetMailvsnetmsghtml

httpwwwkusastrokyotouacjpvsnetMailvsnetmsghtml

httpwwwkusastrokyotouacjpvsnetMailvsnetmsghtml and

httpwwwkusastrokyotouacjpvsnetMailvsnetmsghtml

The author is grateful to the USNO PMM team for making USNO A CDROMs

available to the author This work is partly supp orted by the GrantinAid for Scientic

Research of the Japanese Ministry of Education Science Culture and Sp orts

Reference

Homeister C Astron Nach

IBVS

Table Precise co ordinates of variable stars

RA Decl

Desig source

J

h m s  0 00

NSV : : GSC mean

NSV GSC

NSV GSC mean

NSV GSC

NSV GSC

VX Scl GSC

NSV GSC

NSV GSC mean

NSV GSC mean

SY For GSC mean

NSV GSC

CR Eri GSC

NSV GSC mean

NSV GSC

NSV GSC mean

NSV GSC

VY Dor GSC

NSV GSC

SS Col USNO

ST Col GSC

NSV GSC

HM Pup GSC mean

NSV GSC

V Cen GSC

FR Lup GSC mean

AW Cir GSC

FS Lup GSC mean

YY Aps GSC mean

V Cen USNO

NSV GSC

FU Lup GSC mean

FV Lup GSC

NSV GSC mean

FY Lup GSC

IR Nor GSC

EX Lup USNO

NSV GSC mean

NSV GSC mean

NSV GSC mean

BS Aps GSC mean

NSV GSC

IBVS

Table cont

RA Decl

Desig source

J

h m s  0 00

HO TrA : : GSC mean

V Sco GSC

FW TrA GSC

V Ara GSC

V Ara GSC

V Ara GSC

V Ara GSC

V Sco GSC

V Ara GSC

NSV GSC

NSV GSC

NSV GSC mean

V Ara GSC

V Ara GSC mean

NSV GSC mean

NSV GSC mean

V Ara USNO

V Ara GSC mean

V Ara GSC mean

NSV GSC

NW Pav GSC

PY Tel GSC mean

V Sgr GSC mean

NSV GSC mean

NSV GSC mean

V CrA USNO

NSV GSC mean

V CrA GSC mean

NSV GSC

V Sgr USNO

V CrA GSC

NSV GSC

NSV GSC mean

OU Tel GSC mean

NSV GSC mean

V Sgr GSC

HI Tel GSC mean

DR Pav GSC

HK Tel GSC mean

NSV GSC mean

IBVS

Table cont

RA Decl

Desig source

J

h m s  0 00

V Sgr : : GSC

NSV GSC mean

V Sgr GSC mean

NSV GSC

HL Tel GSC

QR Pav GSC

HM Tel GSC

NSV GSC

V Sgr GSC

FO Pav GSC mean

NSV GSC

NSV GSC

NSV GSC mean

NSV GSC

PP Tel GSC mean

IS Tel GSC mean

SW Ind GSC

V Pav GSC mean

V Pav GSC

NSV USNO

SX PsA GSC mean

NSV GSC

AT Gru GSC mean

SY PsA USNO

NSV GSC mean

SV Gru GSC

AO Ind GSC

AQ Ind GSC

UW Gru GSC mean

AZ Ind GSC

WZ Gru GSC mean

SZ PsA GSC mean

NSV GSC mean

AE Gru GSC

NSV GSC mean

AQ Gru GSC mean

NSV GSC mean

AK Scl GSC mean

NSV GSC

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

September

HU ISSN

PRECISE COORDINATES OF VARIABLE STARS

T KATO

Dept of Astronomy Faculty of Science Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp

This rep ort contains accurate J p ositions for variable stars discovered by

Homeister The variables stars listed in Table were identied against computer

plots of GSC and USNO A catalogs The color information and IRAS PSC identica

tion were also examined in identifying red variables The source of identication in column

Cat G GSC GM average of GSC multiple entries U USNOA UM

average of USNOA multiple entries

V Her S V Ara S V Ara S V CrA S FS Aps

S CY Mus S DX Mus S V Aql S brightest or most

likely candidates are given

V Ara S no go o d candidate Ob ject listed may b e to o faint

DY Mus S p osition corrected in GCVS Comparison with the original article

supp orts the identication in the table

MY Per S NS Per S V Cyg S V Cyg S

V Cyg S identical identications in Downes et al However the

cataloged range of p osition for V Cyg indicates a blank eld on POSS The true

identication should b e checked by astrometry during outburst

Detailed information of identications other catalog identications are available from

the VSNET archive vsnet and

httpwwwkusastrokyotouacjpvsnetMailvsnetmsghtml etc

The author is grateful to the USNO PMM team for making USNO A CDROMs

available to the author This work is partly supp orted by the GrantinAid for Scientic

Research of the Japanese Ministry of Education Science Culture and Sp orts

References

Downes R Webbink R F Shara M M PASP

Homeister C Astron Nach

IBVS

Table Precise co ordinates of variable stars

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

MN Per : : U MO Per : : G

MP Per G MQ Per U

MR Per GM MS Per G

MT Per G MU Per U

V Per U MV Per G

V Per G MY Per U

MZ Per U V Per G

NO Per G V Per G

NQ Per U NS Per U

V Per G V Per G

NT Per U NU Per G

NX Per U AO Cam G

OO Per U OR Per U

OS Per U OT Per U

OU Per U OV Per U

KR Pup GM HQ Cep U

V Cas G V Lac GM

GN Lac G GP Lac U

GR Lac U GT Lac U

FY Lac G GU Lac U

V Her GM V Her GM

V Her G V Her U

V Her U V Her GM

V Her G V Her U

V Her U V Her G

V Her U V Her U

V Her G V Her U

V Her GM V Her G

V Oph U V Her G

V Oph U V Her GM

V Oph U V Oph G

V Her U V Her U

V Oph U V Oph G

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara UM

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara UM

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara UM

V Ara U V Ara U

V Sco U MQ Ara U

V Ara U V Ara U

IBVS

Table cont

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

V Ara : : U V Ara : : G

V Ara U V Ara U

V Ara U V Ara U

V Sco U V Ara U

V Ara G V Ara U

V Ara U V Sco U

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Sco U

V Ara U V Ara U

V CrA U V CrA G

V Ara U V Ara U

V Ara U V Ara U

V Ara UM V Ara U

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara U

V Ara U V Ara U

V CrA U KM Tel U

KN Tel U KP Tel U

KO Tel U V CrA U

KQ Tel U KR Tel U

V CrA U V CrA U

KS Tel U KT Tel U

V CrA U KU Tel U

KV Tel U KW Tel U

KX Tel U V CrA U

KY Tel U LL Tel U

KZ Tel U LM Tel U

LN Tel U LO Tel U

LP Tel U LQ Tel U

LR Tel U LS Tel U

LT Tel U V CrA U

LU Tel G V CrA U

LV Tel U V CrA U

LW Tel U LX Tel U

LY Tel U MM Tel U

MN Tel U MO Tel U

V CrA GM MP Tel U

MQ Tel U MR Tel U

MS Tel U EU Tel G

FS Aps U BI Cir U

FT Aps U BK Cir U

AY Cir U FF Aps U

AZ Cir U LX Aps U

BL Cir G BM Cir U

BC Cir U EM TrA GM

GU TrA G FG Aps U

FZ Aps U IX TrA U

BH Cir U GG TrA U

IBVS

Table cont

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

GV TrA : : U GH TrA : : U

GW TrA U LZ Aps U

GX TrA U FH Aps U

FI Aps U FK Aps U

GI TrA U FL Aps G

GK TrA U GL TrA U

GM TrA U GY TrA G

FU Aps U FM Aps U

FN Aps GM GO TrA U

GZ TrA G HH TrA U

GP TrA U CU Mus U

CV Mus GM CW Mus G

CY Mus U DP Mus U

CZ Mus G DQ Mus UM

DR Mus G EI Mus G

DD Mus U DE Mus U

DF Mus G DG Mus U

DS Mus U IQ Mus U

DT Mus U DU Mus U

EP Mus GM DH Mus U

DI Mus U DV Mus U

DK Mus U DL Mus U

ER Mus U DM Mus U

DX Mus U DY Mus GM

DN Mus G BY Cha U

V Her U V Her U

V Her G V Her U

V Aql U V Aql U

V Aql U V Aql U

V Aql U V Aql G

V Aql U LL Vul U

NW Vul U LM Vul U

LN Vul U LQ Vul U

LR Vul U LS Vul U

V Cyg U V Cyg U

V Cyg U V Cyg U

V Cyg U V Cyg U

V Cyg U V Cyg U

V Cyg U V Cyg U

V Cyg U V Cyg U

V Cyg U V Cyg U

V Cyg U AN Cyg U

V Cyg U V Cyg G

V Cyg U V Cyg U

V Cyg U V Cyg U

V Cyg U V Cyg U

V Cyg U V Cyg U

V Cyg U V Cyg U

V Cyg U V Cyg U

V Cyg G

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

September

HU ISSN

CCD PHOTOMETRY OF THE FEBRUARY SUPEROUTBURST OF

CY UMa

T KATO K MATSUMOTO

Dept of Astronomy Kyoto University Kyoto Japan email tkatokusastrokyotouacjp

CY UMa was discovered as a dwarf nova by Goranskij Following the initial

claim of visual and photographic sup erhump detection by Kato et al CCD obser

vations indep endently revealed the presence of sup erhumps Kato Harvey Patterson

During the February sup eroutburst starting on February E Muyllaert

m VSNET we underto ok timeresolved CCD photometry of CY UMa

v

The observations were done using an unltered ST camera attached to the Meade

cm SchmidtCassegrain telescop e The exp osure time was s The images were dark

TM

subtracted atelded and analyzed using the Java based ap erture and PSF photome

try package developed by one of the authors TK The ux of the variable was measured

relative to GSC Tycho V B V USNO r magnitude

whose constancy was conrmed by comparison with GSC USNO r magnitude

Figure illustrates the overall light curve of the present observation Before February

JD individual observations are plotted after the decline nightly averages

with error bars are plotted instead The sup eroutburst plateau stage February

was analyzed after subtracting the linear decline trend mag d using the Phase

Disp ersion Minimization PDM metho d Stellingwerf

The result of p erio d analysis is given in Figure Although unavoidable oneday aliases

exist we can safely choose with the help of previous p erio d determinations the correct

p erio d of  d corresp onding to the frequency of d The present

b est p erio d agrees with previous rep orts within resp ective errors  d Kato

and  d Harvey Patterson

Besides sup erhumps we examined the p ostsup eroutburst b ehavior during which some

SU UMatype dwarf novae are known to show rebrightenings No evidence of rebrightening

was observed b oth in our CCD monitoring until d past the steep decline and visual

monitoring rep orted to VSNET

Figure shows enlarged light curves of nightly runs The typical error of a single

measurement was mag on February and mag on other nights The amplitude

of sup erhumps was the largest mag on February and gradually decayed On

the declining branch from the sup erhump maximum on February quasip erio dic oscil

lations QPOs with a p erio d of m were visible This mo dulation quickly decayed

on subsequent nights

IBVS

2 CY UMa (1999 February)

4

6 Relative magnitude Relative

8

25 30 35 40 45

HJD - 2451200

Figure Overall light curve of CY UMa

1.1

1

.9

.8 theta .7

.6

.5 P = 0.0722 .4 10 11 12 13 14 15 16 17 18

Frequency (cycle/day)

Figure Period analysis of CY UMa

IBVS

0

Feb. 13 .5

Feb. 14

1 Feb. 15 Relative magnitude 1.5 Feb. 16

Feb. 19 2

-.1 -.05 0 .05 .1

Fraction of HJD

Figure Nightly light curve of CY UMa

IBVS

The authors are grateful to VSNET observers who rep orted timely visual observations

This work is partly supp orted by the GrantinAid for Scientic Research of

the Japanese Ministry of Education Science Culture and Sp orts TK Part of this work

is supp orted by a Research Fellowship of the Japan So ciety for the Promotion of Science

for Young Scientists KM

References

Goranskij V P Astron Tsirk No

Harvey D Patterson J PASP

Kato T IBVS No

Kato T Fujino S Iida M Makiguchi N Koshiro M VSOLJ Variable Star

Bul letin

Stellingwerf R F ApJ

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

September

HU ISSN

PRECISE COORDINATES OF VARIABLE STARS

T KATO

Dept of Astronomy Faculty of Science Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp

This rep ort contains accurate J p ositions for variable stars discovered by

Homeister The variable stars listed in Table were identied against computer

plots of GSC and USNO A catalogs The color information and IRAS PSC identi

cation were also examined in identifying red variables The source of identication in

column Cat G GSC GM average of GSC multiple entries U USNO

A UM average of USNO A multiple entries

PY Per S correctly identied in Downes et al Known to have a close

th mag companion

V Per S Downes et al p oints a USNO star probably close to the

real ob ject however Homeisters description corresp onds to a blank region on POSS

We should probably need further astrometry during outburst

KZ Gem S identication in Downes et al probably correct Co ordinates

given corresp ond to those by Downes et al

V Lyr S app ears very bright b oth on GSC and USNO A Homeisters

plot suggests a bright star which is in conict with the rep orted range of variability

m by Homeister

pg

V Cas S double star in USNO no mentioning by Homeister Redder

comp onent given

Detailed information of identications other catalog identications are available from

the VSNET archive vsnet

httpwwwkusastrokyotouacjpvsnetMailvsnetmsghtml etc

The author is grateful to the USNO PMM team for making USNO A CDROMs

available to the author This work is partly supp orted by the GrantinAid for Scientic

Research of the Japanese Ministry of Education Science Culture and Sp orts

References

Downes R Webbink R F Shara M M PASP

Homeister C Astron Nach

IBVS

Table Precise co ordinates of variable stars

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

V Cas : : U V Cas : : G

V Cas G V Cas GM

V Cas U V Cas U

V Cas U V Cas G

V Cas G OY Per U

V Cas U V Cas G

V Cas G V Cas UM

V Per G V Per G

PW Per U V Per G

PX Per U V Per G

V Per GM V Per U

PY Per U V Per U

V Per G V Per G

V Per U V Per G

QS Per U V Per G

QU Per G V Per U

V Per G QV Per G

V Per G V Per GM

QW Per G V Per GM

V Per U QX Per GM

V Per G V Tau GM

LZ Aur G MM Aur U

IZ Tau U V Tau G

MQ Aur U MS Aur G

LR Aur U LN Gem GM

LQ Gem U V Ori U

V Ori U IX Gem U

IZ Gem U KL Gem U

KW Gem U KU Gem U

KX Gem U KZ Gem U

MR Gem U LL Gem U

LM Gem U NO Gem G

AS CMi U AT CMi U

AU CMi U LU Pup G

CC Leo U BY Com U

DD Vir U CF Com U

CS Com U CW Com G

DE Com U DH Com G

DN Com U DQ Com U

DZ Com G DP Vir U

DF Vir U V Her U

IBVS

Table cont

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

V Her : : U V Her : : U

V Her U V Her G

V Her U V Her U

V Her U V Her U

V Her U V Her G

V Her G V Her U

V Her U V Her G

V Her G V Oph U

V Oph G V Oph U

V Oph G V Oph U

V Oph U V Oph U

FF Ser G V Oph U

V Oph U V Oph U

V Oph U V Oph U

V Oph U V Oph UM

V Oph U V Oph G

V Oph U V Oph GM

V Oph GM V Oph U

V Oph U V Oph U

V Oph U V Oph U

V Her U V Her U

V Her U V Her U

V Her U V Her U

V Lyr UM V Lyr G

V Lyr U V Lyr G

V Lyr G V Lyr U

V Lyr U V Lyr G

V Her U V Lyr U

V Lyr U V Lyr U

V Lyr U V Lyr U

V Lyr U V Lyr U

V Lyr U V Lyr U

V Lyr U V Lyr G

V Lyr U V Lyr GM

V Lyr U V Lyr U

V Lyr G V Cyg U

V Lyr G V Cyg U

V Cyg U BZ Dra U

DT Dra G CD Dra U

CE Dra U CF Dra G

CG Dra U V Cyg U

IBVS

Table cont

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

V Cyg : : U V Cyg : : U

V Cyg U V Cyg U

V Cyg U V Cyg U

V Cyg UM CI Dra U

V Cyg U V Cyg UM

V Cyg U V Cyg U

V Cyg U V Aql G

V Aql U V Aql G

V Aql U V Aql G

V Aql U V Aql U

V Aql U V Aql U

V Aql U V Aql U

V Aql G V Aql U

V Aql U V Aql GM

V Aql G V Aql U

V Aql U V Aql U

V Aql GM V Aql U

V Aql U V Aql G

V Aql G V Aql U

V Aql U V Aql U

V Aql U V Aql U

V Aql U V Aql GM

V Aql U V Aql U

V Aql U V Aql GM

V Aql G V Aql U

V Aql U V Aql GM

V Aql U V Aql UM

V Aql U V Aql U

V Aql G V Aql GM

V Aql U V Aql U

V Aql U V Aql U

V Aql GM V Aql U

V Aql U V Aql U

V Aql U V Aql U

V Aql GM V Aql U

V Aql G V Aql U

V Aql U V Aql GM

V Aql U V Aql U

V Cyg G V Cyg G

V Cyg U V Cyg G

V Cas U V Cas G

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

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September

HU ISSN

CCD OBSERVATION OF THE OCTOBER SUPEROUTBURST

OF PU Per CONFIRMATION AS AN SU UMaTYPE DWARF NOVA

T KATO K MATSUMOTO

Dept of Astronomy Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp katsurakusastrokyotouacjp

PU Per is a dwarf nova discovered by Homeister The historical record of

outbursts suggesting the SU UMatype is reviewed in Kato and Nogami Kato

and Nogami made timeresolved photometry of the short outburst in Octob er

On the rapidly decaying stage of the outburst they detected p ossible humplike features

with a p erio d of  d The conrmation of the SU UMatype nature has b een thus

awaited for

On September T Kinnunen rep orted the detection of a bright m

v

outburst Up on this alert we observed PU Per on three nights of Octob er The

observations were done using an unltered ST camera attached to the Meade cm

SchmidtCassegrain telescop e The exp osure time was s The images were dark

TM

subtracted atelded and analyzed using the Java based PSF photometry package

developed by one of the authors TK The ux of the variable was measured relative to

GSC USNO r magnitude whose constancy was conrmed by comparison

with GSC USNO r magnitude The uxes given in gures of this note

are expressed relative to GSC

Figure illustrates the overall light curve of the present observation The light curve

shows a steady decline characteristic of sup eroutbursts After subtracting the linear de

clining trend the light curve was analyzed using the Phase Disp ersion Minimization

PDM metho d Stellingwerf and LANCELOT p erio d analysis using articial neu

ral networks Gaspani ab The resultant theta diagram PDM and Gf function

LANCELOT are shown in Figure The minimum and maximum p oints resp ectively

corresp ond to the b est estimates of the p erio d

The selection of the b est sup erhump p erio d suers from some diculties owing to

the low signaltonoise ratio and the gaps caused by clouds From the three oneday

alias candidate p erio ds and d we have chosen the p erio d 

corresp onding to the frequency of d as the b estdetermined p erio d based

on the indep endent sup erhump detection information Kemp and Vanmunster private

communication However there still remains the p ossibility for other aliases from the

present data set

IBVS

.06 PU Per (1998 October)

.05

.04

.03 Relative flux .02

.01

0

89 89.5 90 90.5 91 91.5

HJD - 2451000

Figure Overall light curve of PU Per

1.02 PDM

1

.98 theta .96

.94

.92 2·10-8 neural network

1.5·10-8

G(f) 10 -8

5·10-9

0 11 12 13 14 15 16 17

frequency

Figure Period analysis of PU Per

IBVS

.004

.002

0 Flux modulation

-.002

-.4 -.2 0 .2 .4 .6 .8 1 1.2 1.4

Superhump phase

Figure Sup erhump prole of PU Per

Figure shows the averaged sup erhump prole folded by the p erio d of d The

mean sup erhump amplitude is  magnitude PU Per can now b e safely classied as

an SU UMatype dwarf nova

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture and Sp orts TK Part of this

work is supp orted by a Research Fellowship of the Japan So ciety for the Promotion of

Science for Young Scientists KM

References

Gaspani A a GEOS Fiche Technique No

Gaspani A b in Proceedings of the th Conference on Variable Star Research

Brno p

Homeister C Astron Nach

Kato T Nogami D IBVS No

Stellingwerf R F ApJ

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

September

HU ISSN

CYCLIC VARIABILITY OF V Aql

T KATO D NOGAMI H BABA

Dept of Astronomy Kyoto University Kyoto Japan email tkatokusastrokyotouacjp

V Aql originally discovered as an irregular variable has b een regarded as a Z Cam

type dwarf nova Meinunger Vogt and Bateson Pastukhova and Shugarov

dealed with the longterm b ehavior of this star showing the presence of o ccasional

fadings Downes et al presented lowresolution sp ectroscopy which supp orted the

cataclysmic nature of the star but the p ossibility of b eing a Herbig AeBe star remained

Masetti and Della Valle obtained timeresolved CCD photometry which indicated

p ossible orbital p erio ds of or hr

Our observations were done using a CCD camera Thomson TH  pixels

onchip  binning adopted attached to the Cassegrain fo cus of the cm reector

fo cal length m at Ouda Station Kyoto University Ohtani et al An

interference lter was used which had b een designed to repro duce the Johnson V band

The exp osure time was s dep ending on the transparency of the sky The frames

were rst corrected for standard debiasing and at elding and were then pro cessed by

a micro computerbased automaticap erture photometry package developed by one of the

authors TK The relative V magnitudes of the variable were determined against GSC

whose magnitude was determined as V using the lo cal comparison stars

by Misselt The constancy of the comparison was conrmed using GSC

V The summary of observations is given in Table

The overall light curve is given in Figure The light curve shows the quasip erio dic

cyclic variation with a p erio d of  d and an amplitude of mag The coverage by

Pastukhova and Shugarov was not dense enough to clearly illustrate this mo dula

tion Though the p erio d of the mo dulation is close to that typical of Z Camtype dwarf

novae the amplitude is rather small The presence of short excursions to faint states

Pastukhova and Shugarov is also unusual for Z Camtype dwarf novae However

the light mo dulation is reminiscent of FY Vul which b ears sp ectroscopic similarity to

V Aql Downes et al There may b e a previously unrecognized group of low

amplitude dwarf novae The Herbig AeBe classication may b etter explain the presence

of o ccasional fadings and the p ossibly asso ciated nebulosity Masetti and Della Valle

but mag cyclic variation seems to b e unusual for this class of ob jects Another

ob ject exhibiting similar activities is FY Per whose cyclic variations with a typical p erio d

of d and a full amplitude of  mag have b een recently established Watanabe

and Maehara and whose nature has b een also discussed as either a cataclysmic

variable or a Herbig AeBe star Okazaki More observations are needed to clarify

the nature of this intriguing ob ject

IBVS

Table CCD observation of V Aql

a a b c d

JD start JD end mag error N

a

JD

b

Magnitude relative to GSC

c

Standard error of nightly average

d Number of frames

IBVS

1.6

V1101 Aql 1.8

2

2.2 magnitude

V

2.4 Relative

2.6

2.8

290 300 310 320 330 340

JD - 24500000

Figure Light curve of V Aql

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture and Sp orts

References

Downes R Hoard H W Szkody P Wachter S AJ

Masetti N Della Valle M Astron Astrophys

Meinunger L Mitt Verand Sterne

Misselt K A PASP

Ohtani H Uesugi A Tomita Y Yoshida M Kosugi G Noumaru J Araya S

Ohta K Memoirs of the Faculty of Science Kyoto University Series A of

Physics Astrophysics Geophysics and Chemistry

Okazaki A Astrophys Space Sci

Pastukhova E N Shugarov S Y Perem Zvezdy

Vogt N Bateson F M Astron Astrophys Suppl

Watanabe T Maehara H VSOLJ Variable Star Bul letin in press

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

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September

HU ISSN

CCD PHOTOMETRY

OF THE DECEMBER OUTBURST OF AQ Eri

T KATO K MATSUMOTO

Dept of Astronomy Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp katsurakusastrokyotouacjp

AQ Eri is an SU UMatype dwarf nova Kato whose sup erhump p erio d was

d

rep orted to b e Thorstensen et al yield a sp ectroscopic orbital p erio d of

d

which places AQ Eri among short orbital p erio d systems The relatively short

orbital p erio d and the relative low frequency of outbursts make AQ Eri a candidate for

an intermediate system b etween usual SU UMatype dwarf novae and WZ Sgetype stars

cf Nogami et al for the discussion of CT Hya

The outburst was detected by Hers on December at m The

v

lack of detected sup eroutburst since and the brightness of the outburst prompted

our timeseries CCD observations

The observations were done using an unltered ST camera attached to the Meade

cm SchmidtCassegrain telescop e The exp osure time was s The images were dark

TM

subtracted atelded and analyzed using the Java based PSF photometry package

developed by one of the authors TK The magnitudes of the variable was measured

relative to GSC Tycho V B V whose constancy was

conrmed by comparison with GSC V B V Table

summarizes the observations

Figure illustrates the overall light curve of the present observation Nightly averaged

relative magnitudes and estimates of errors are plotted for the last two nights The light

curve shows a steep decline characteristic of a normal outburst The data of the rst

two nights when the variable was in outburst were analyzed after subtracting the linear

declining trend using the Phase Disp ersion Minimization PDM metho d Stellingwerf

The result gave no very convincing p erio dicity but seemed to have a weak signal

around the rep orted orbital p erio d and not around the sup erhump p erio d

In order to more closely examine the p otential orbital mo dulation the data of the rst

two nights were phaseaveraged using the rep orted p erio d of d The result is

shown in Figure which shows the existence of a doublewave mo dulation in one orbital

cycle The amplitude of the mo dulation was  mag The data on December

the third night were analyzed in the same way giving the upp er limit of the orbital

mo dulation of  mag indicating that the mo dulation during outburst decayed as the

system faded It is noteworthy that similar doubly humped orbital mo dulations during

early outburst have b een observed in the early stage of WZ Sgetype outbursts and are considered as one of dening characteristics of WZ Sgetype phenomenon eg Matsumoto

IBVS

3

AQ Eri 4 (1998 December)

5 Relative magnitude

6

7 66 67 68 69 70 71 72

HJD - 2451100

Figure Overall light curve of AQ Eri

Table Summary of observations

a a b

JD start JD end N

a

JD

b Number of frames

IBVS

AQ Eri outburst orbital variation

-.1

-.05

0 Relative magnitude

.05

.1

-.4 -.2 0 .2 .4 .6 .8 1 1.2 1.4

Phase

Figure Hump prole of AQ Eri

et al The present outburst of AQ Eri may have b een followed the similar course

of WZ Sgetype outburst but failed to trigger a sup eroutburst More extensive studies

of outbursts of similar systems with infrequent outbursts are thus encouraged

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture and Sp orts TK Part of this

work is supp orted by a Research Fellowship of the Japan So ciety for the Promotion of

Science for Young Scientists KM

References

Hers J VSNET alert circulation No also available from

httpwwwkusastrokyotouacjpvsnetMailvsnetalertmsghtml

Kato T IBVS No

Matsumoto K Nogami D Kato T Baba H PASJ

Nogami D Kato T Hirata R PASJ

Stellingwerf R F ApJ

Thorstensen J R Patterson J Shambrook A Thomas G PASP

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

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September

HU ISSN

CCD PHOTOMETRY OF THE MARCH OUTBURST OF BZ UMa

DETECTION OF QUASIPERIODIC OSCILLATIONS

T KATO

Dept of Astronomy Kyoto University Kyoto Japan email tkatokusastrokyotouacjp

d

BZ UMa is a dwarf nova whose orbital p erio d has b een determined as Ringwald

et al Jurcevic et al Although the orbital p erio d shorter than the p erio d gap

strongly suggests the SU UMatype classication no conrmed sup eroutburst has b een

yet observed Jurcevic et al

Up on the alert of a bright outburst on March reaching m Muyllaert

v

we started timeresolved CCD photometry The outburst rivaled the brightest

recorded historical outbursts cf Jurcevic et al

-1 BZ UMa 0

1

2

3 Relative magnitude

4

5

48 49 50 51 52 53 54 55

HJD - 2451200

Figure Overall light curve of BZ UMa

IBVS

The observations were done using an unltered ST camera attached to the Meade

cm SchmidtCassegrain telescop e The exp osure time was s The images were dark

TM

subtracted atelded and analyzed using the Java based PSF photometry package

developed by the author The dierential magnitudes of the variable were measured

against GSC USNO r magnitude whose constancy was conrmed by

comparison with GSC USNO r magnitude

The overall light curve is shown in Figure The magnitudes are given relative to

GSC The outburst was despite its brightness a short rapidly fading one No

detectable sup erhumps were observed However on its decline the ob ject showed unusual

short timescale oscillations Figure shows the b est exemplication of the wave the rst

fragment of the March run

2.2 BZ UMa

2.4

2.6

2.8

3 Relative magnitude

3.2

3.4

49.92 49.94 49.96 49.98 50 50.02

HJD - 2451200

Figure Enlarged light curve on March

d

The p erio d of mo dulations was close to the amplitude of the signal was as large as

m

the prole was doublewaved to this p erio d Figure shows the result of the p erio d

analysis by applying the Phase Disp ersion Minimization PDM metho d Stellingwerf

to the March data after removing the longterm trend The b est p erio d was

d

but as is evident from the broad signal in the theta diagram the mo dulations

were quasip erio dic in nature Sup erp osition of dierent p erio dicities is also p ossible

The signicant deviation from the orbital p erio d may suggest that the mo dulation can

b e caused by the intermediate p olar or QPOlike phenomenon The relative strength

of highexcitation lines Ringwald et al Jurcevic et al and the relatively

strong Xray emission RXS J may also supp ort a weakly magnetic

white dwarf If the intermediate p olar nature of BZ UMa can b e conrmed by future

observations it may b e a clue to understanding the apparent lack of sup eroutbursts

IBVS

1.05

1

.95

.9 theta

.85

.8 P = 0.0271

.75 10 15 20 25 30 35 40 45 50

Frequency (cycle/day)

Figure Periodogram of BZ UMa

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture and Sp orts

References

Jurcevic J S Honeycutt R K Schlegel E M Webbink R F PASP

Muyllaert E vsnet alert circulation No also available at

httpwwwkusastrokyotouacjpvsnetMailvsnetalertmsghtml

Ringwald F A Thorstensen J R Hamway R M MNRAS

Stellingwerf R F ApJ

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

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September

HU ISSN

ORBITAL MODULATION DURING THE STANDSTILL OF VW Vul

T KATO

Dept of Astronomy Kyoto University Kyoto Japan email tkatokusastrokyotouacjp

Since the work by Shafter VW Vul had long b een susp ected as an ultrashort

orbital p erio d d dwarf nova until the correct orbital p erio d  d

was revealed by Thorstensen et al The new orbital p erio d is consistent with the

observed presence of standstills which are a signature of Z Camtype dwarf novae

During the standstill of VW Vul we p erformed timeresolved CCD photometry

initially intending the detection of p ossible p erio dicity asso ciated with the claimed short orbital p erio d

-.2 VW Vul -.1

0

.1 magnitude

V .2 Relative .3

.4

1 2 3 4 5

HJD - 2450000

Figure Light curve of VW Vul during the standstill

The observations were done on ve successive night b etween Octob er and

using a CCD camera Thomson TH  pixels onchip  binning adopted

IBVS

attached to the Cassegrain fo cus of the cm reector fo cal length m at Ouda

Station Kyoto University Ohtani et al An interference lter was used which had

b een designed to repro duce the Johnson V band The exp osure time was s The frames

were rst corrected for standard debiasing and at elding and were then pro cessed by

a micro computerbased automaticap erture photometry package developed by the au

thor The relative V magnitudes of the variable were determined against USNOA

h m s  0 00

J whose magnitude was determined as

V using the lo cal comparison stars by Andronov et al The constancy of

the comparison was conrmed using GSC Figure illustrates the overall light

curve The observed averaged magnitude during this standstill was V

VW Vul

1

.95 theta

.9

P = 0.1676

.85 5.4 5.6 5.8 6 6.2 6.4 6.6

Frequency (1/d)

Figure Period analysis of VW Vul

The light curve was analyzed using the Phase Disp ersion Minimization PDM metho d

Stellingwerf The theta diagram is shown in Figure While oneday aliases are

unavoidable due to the limited run lengths the existence of p erio dicity very close to

the orbital p erio d strongly implies the presence of orbital mo dulation The signicance

level of the p erio d is using Ftests The b est p erio d assuming this alias selection

determined from the PDM analysis is  d The p erio d is very close to the

orbital p erio d but can b e  shorter

The folded hump prole by the d p erio d is shown in Figure The prole is

singly p eaked suggesting the orbital humps as the origin The amplitude of the hump

is  mag The ep o chs of hump maxima during this p erio d can b e expressed by the

following ephemeris

d

MaxHJD  E

IBVS

-.1

VW Vul (P = 0.1676 d)

-.05

magnitude 0 V Relative

.05

.1 -.4 -.2 0 .2 .4 .6 .8 1 1.2 1.4

Photometric phase

Figure Hump prole of VW Vul

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture and Sp orts

References

Andronov I L Boro dina I G Kolesnikov S V Shakhovskoy N M Shvechkova N

A IBVS No

Ohtani H Uesugi A Tomita Y Yoshida M Kosugi G Noumaru J Araya S

Ohta K Memoirs of the Faculty of Science Kyoto University Series A of

Physics Astrophysics Geophysics and Chemistry

Shafter A W AJ

Stellingwerf R F ApJ

Thorstensen J R Taylor C J Kemp J PASP

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

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September

HU ISSN

NEW VARIABLE STARS DISCOVERED IN THE MISAO PROJECT

I I MisVMisV

SEI ICHI YOSHIDA KENICHI KADOTA TAICHI KATO

1

MISAO Pro ject Miyawada Fujishiromachi Kitasomagun Ibaraki Japan

email seiichimuraokainfowasedaacjp

2

MISAO Pro ject Koshikiya Ageo City Saitama Japan

email kenickastroartscojp

3

Dept of Astronomy Kyoto University Kyoto Japan email tkatokusastrokyotouacjp

This rep ort describ es new variable stars MisVMisV discovered in the

course of the MISAO Pro ject

These ob jects are detected automatically by the PIXY system as candidates of variable

stars from unltered CCD images taken by Kadota b etween March and August then

conrmed by Yoshida and Kadota Further details are same as describ ed in Yoshida and

Kadota

The list of new variable stars is given in Table The p osition and magnitude

are measured with USNOA catalog The magnitude is based on a preliminary V

magnitude calculated from R and B magnitude in the catalog based on Katos

equation

V R B R

The nding charts are available electronically as fnnneps where nnn refers to the

serial number assigned to the star in the rst column of Table

MisV is arcsec from V Cyg a rapidly changing irregular variable at

h m s  0 00

RA Decl in the GCVS But MisV is identied

with IRAS so it is probably Mira type or semiregular type Considering the

large distance and the type dierence we concluded that MisV is another new vari

able star However no star brighter than mag was detected on our unltered CCD

images taken on JD and at the p osition

of V Cyg Therefore it cannot b e completely ruled out that the p osition of V

Cyg is inaccurate and MisV is identical with V Cyg

MisV is identied with HS one of the variable stars discovered by FASTT

Flagsta Astrometric Scanning Transit Telescope cf Henden and Stone

NSV is arcmin from MisV No star brighter than mag was detected

at the p osition of NSV on our unltered CCD images taken on JD

and However considering the large angular distance MisV

is probably another variable ob ject

IBVS

References

Henden A A Stone R C AJ

Kato T

httpwwwkusastrokyotouacjpvsnetMailvsnetchatmsghtml

Yoshida S Kadota K IBVS No

Yoshida S in preparation

Table List of New Variable Stars

Unltered

Co de RA J Decl CCD Mag Type Identied with

Max Min

h m s  0 00

MisV : :

MisV

MisV

MisV USNOA

MisV

MisV USNOA

MisV

MisV USNOA

IRAS

MisV IRAS

MisV IRAS

MisV IRAS

MisV USNOA

IRAS

MisV IRAS

MisV IRAS

MisV GSC

USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

MisV GSC

USNOA

IRAS

MisV USNOA

MisV USNOA

IRAS

MisV USNOA

IBVS

Table cont

Unltered

CCD Mag

Co de RA J Decl Type Identied with

Max Min

h m s  0 00

MisV : : USNOA

IRAS

MisV USNOA

IRAS

MisV GSC

USNOA

MisV USNOA

MisV USNOA

IRAS

HS

MisV IRAS

MisV SR IRAS

MisV USNOA

IRAS

MisV IRAS

MisV SR IRAS

MisV IRAS

MisV SR USNOA

IRAS

MisV

MisV

MisV USNOA

MisV

MisV USNOA

MisV USNOA

MisV USNOA

MisV USNOA

MisV

MisV USNOA

IRAS

MisV

MisV SR IRAS

MisV USNOA IRAS

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

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September

HU ISSN

NEW VARIABLE STARS DISCOVERED IN THE MISAO PROJECT

I I I MisVMisV

SEI ICHI YOSHIDA KENICHI KADOTA TAICHI KATO

1

MISAO Pro ject Miyawada Fujishiromachi Kitasomagun Ibaraki Japan

email seiichimuraokainfowasedaacjp

2

MISAO Pro ject Koshikiya Ageo City Saitama Japan

email kenickastroartscojp

3

Dept of Astronomy Kyoto University Kyoto Japan email tkatokusastrokyotouacjp

This rep ort describ es new variable stars MisVMisV discovered in the

course of the MISAO Pro ject

These ob jects are detected automatically by the PIXY system as candidates of variable

stars from unltered CCD images taken by Kadota b etween April and August then

conrmed by Yoshida and Kadota Further details are same as describ ed in Yoshida and

Kadota

Here is the list of new variable stars Table The p osition and magnitude are mea

sured with USNOA catalog The magnitude is based on a preliminary V magnitude

calculated from R and B magnitude in the catalog based on Katos equation

V R B R

The nding charts are available electronically as fnnneps where nnn refers to the

serial number assigned to the star in the rst column of Table

MisV is identied with a carb on star CS

V Cyg is arcmin from MisV V Cyg was detected on our unltered

CCD images at around mag No variability was found on our images However

considering the large distance MisV is probably another new variable star

References

Yoshida S Kadota K IBVS No

Yoshida S Kadota K Kato T IBVS No

Yoshida S in preparation

Kato T httpwwwkusastrokyotouacjpvsnetMailvsnetchatmsghtml

IBVS

Table List of New Variable Stars

Unltered

CCD Mag

Co de RA J Decl Type Identied with

Max Min

h m s  0 00

MisV : : SR USNOA

IRAS

MisV GSC

USNOA

IRAS

MisV IRAS

MisV USNOA

IRAS

MisV SR USNOA

IRAS

MisV SR USNOA

IRAS

MisV M USNOA

IRAS

MisV USNOA

IRAS

MisV IRAS

MisV IRAS

MisV SR IRAS

MisV SR IRAS

MisV IRAS

CS

MisV IRAS

MisV IRAS

MisV IRAS

MisV IRAS

MisV USNOA

IRAS

MisV USNOA

MisV IRAS

MisV USNOA

IRAS

MisV IRAS

MisV SR USNOA

IRAS

MisV USNOA

IRAS

MisV SR USNOA IRAS

IBVS

Table cont

Unltered

Co de RA J Decl CCD Mag Type Identied with

Max Min

h m s  0 00

MisV : : IRAS

MisV IRAS

MisV IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV IRAS

MisV IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV IRAS

MisV IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV IRAS

MisV IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV IRAS

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

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September

HU ISSN

A NEW CLASSICAL CEPHEID IN SAGITTA

SV ANTIPIN

Sternberg Astronomical Institute Universitetskij Prosp Moscow Russia

email antipinsaimsuru

Name of the ob ject

Var GSC

Equatorial co ordinates Equinox

h m s  0 00

RA DEC J

Observatory and telescop e

cm astrograph in Crimea

Detector Photoplate

Filters None

Comparison stars See Fig

Check stars None

Transformed to a standard system B

pg

Standard stars eld used B band standard sequence in NGC

Hoag et al

Availability of the data

Up on request

Type of variability DCEP

Remarks

The star was estimated on plates taken during JD Periodic

variability with a light curve typical of a classical Cepheid was found The light

elements are the following

d

JD  E

max

m m p

The range of variability is M m

Acknowledgements

This study was supp orted in part by the Russian Foundation for Basic Research and

the Council of the Program for the Supp ort of Leading Scientic Schools through

grants Nos and

IBVS

Figure The nding chart and the comparison stars

Figure The phased light curve Uncertain estimates are shown as op en circles

Reference

Hoag AA Johnson HL Iriarte B Mitchell RI Hallam KL Sharpless S

Publ of the US Naval Obs vol XVI I part VI I Washington

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

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HU ISSN

LOST VARIABLES ON NANTUCKET PLATES

1;2 3;2 4;2 5;2 6;2

NN SAMUS L HAYTHE S HORNSTEIN LJ JISONNA JR E LU

1

Institute of Astronomy Russian Academy of Sciences Pyatnitskaya Str Moscow Russia

samussaimsusu

2

Maria Mitchell Observatory Vestal Str Nantucket MA USA

3

American School in London London UK mo onaolcom

4

Virginia Polytechnical Institute and State University Miles Hall Blacksburg VA USA

shornstevtedu

5

University of Arizona Tucson AZ USA ljjuarizonaedu

6

Wesleyan University Box Church Str Middletown CT USA eluwesleyanedu

For the reasons discussed by Hazen and Samus it is imp ortant to recover

Harvard variables lacking nding charts This problem can b e most eectively solved

using the Harvard plate collection where many plates still hold ink marks left by the

discoverers However much can b e done using plate collections of other observatories

In particular the plate collection of the Maria Mitchell Observatory MMO containing

esp ecially many plates of the Scutum cloud can b e used with success to recover lost

Harvard variables in this part of the sky

In we have successfully recovered lost Harvard variable stars on Nantucket

plates The main results are presented in Tables and The columns of Table

contain GCVS name preliminary Harvard designation HV Harvard Variable GSC

number if available the stars right ascension and declination equinox source

of co ordinates A means the US Naval Observatory A catalog Monet et al

DSS means co ordinates measured by us on a DSS image relative to several reference

stars with co ordinates from the USNO A catalog The columns of Table contain

GCVS name the stars type found in our study light elements ep o ch and p erio d if they

could b e derived from our Nantucket and Moscow data ep o chs refer to minimum light

for eclipsing variables and to maximum light for other types for Algols the elements are

helio centric

We would like to discuss the case of one more star the lost Cepheid IU Aql in

m m

greater detail It was discovered by Walton as varying b etween and on

Nantucket plates Walton writes that at the MMO plates of the M region were

taken in of them showing stars of magnitude or fainter obviously

to o optimistic an opinion ab out old Nantucket plates Harwoo d classied the star

as a p ossible Cepheid with light elements

d

Max JD  E

Near the p osition given by Walton there is only one star bright enough namely GSC

h m s  0 00

The only published nding chart Bateson

IBVS

et al is not suciently detailed but do es not contradict the ab ove GSC identica

tion However this GSC star is denitely not a Cepheid and probably do es not vary at

all according to mo dern photo electric and CCD data Berdnikov

Table Identications and Co ordinates

Name HV GSC Source

: :

h m s  0 00

BC Sgr GSC

BY Sgr A

CU Sgr A

UW Sct GSC

ZZ Sct A

AE Sct A

BC Sct DSS

Table Types and Light Elements

Name Type Ep o ch JD Period

d

BC Sgr M

BY Sgr SR

CU Sgr SR  yr

UW Sct LB

d

ZZ Sct EA

d

AE Sct EA

d

BC Sct M

Notes on individual stars

BC Sgr The provisional elements in Table are based on maxima after JD

ZZ Sct Elements have b een slightly mo died from those published by Delhaye

taking into account timings of fadings on Moscow plates and one comparatively recent

fading on Nantucket plates

AE Sct We have found the star faint on plates JD these fadings

are in p o or agreement with the light elements from Oosterho Our new elements

d

see Table give O C for Oosterho s ep o ch so the p erio d has

probably really changed

BC Sct According to the discoverer Cannon the following star in a close pair

varies The star found variable on MMO plates is denitely a pair in the DSS Its following

comp onent not contained in the USNO A catalog is red and comparatively faint on

POSS prints whereas it is brighter than the preceding comp onent in the DSS The ep o ch

of the DSS plate JD nearly coincides with the brightest maximum observed by

us JD

IBVS

The MMO p ossesses a copy of a PhD dissertation by Marjorie Williams contain

ing some unpublished results of probably the last study of IU Aql on Nantucket plates A

photographic nding chart in the dissertation clearly identies IU Aql with the star now

known as GSC No individual measurements are given for the star and the

conclusion is the following

IU Aql At rst this star was thought to have a p erio d of less than one day and later

was thought to b e a Cepheid with a p erio d of ab out days Only observations were

made in the present study and it is felt that they are not very reliable as the star was

usually near the edge of the plates and the images were diuse Not enough observations

in one day were obtained to tell whether it is a clustertype or a typical Cepheid

We have lo cated Dr Williamss working noteb o oks at the MMO Most estimates show

m

IU Aql fainter than Williams estimated it brighter only on plates We have

reexamined these plates and at least for of them could not reliably conrm the

maximum We conclude that the MMO plates studied by Williams show few maxima if

any and do not denitely conrm variability Harwoo d must have studied IU Aql

on Harvard not MMO plates b ecause her light elements give the initial maximum not

represented in the MMO plate collection and IU Aql is not mentioned in M Harwoo ds

MMO noteb o oks Either the actual variable was lost so on after Harwoo ds study or it

ceased variations as early as in the ies M Walton Mayalls MMO noteb o ok found

by Dr V Strelnitski do es not contain nding charts

Thanks are due to Vladimir Strelnitski for his help and attention This study was

supp orted in part by grants from the National Science Foundation AST and

from Russian Foundation for Basic Research

References

Bateson FM et al Charts for Southern Variables Ser Chart

Berdnikov LN Private communication

Cannon AJ Harvard Obs Circ No

Delhaye J Bull Astron Inst Netherl

Harwoo d M Harvard Obs Bull No

Hazen ML Samus N IBVS No

Monet D Bird A Canzian B et al USNO A V A Catalog of Astrometric

Standards US Naval Observatory CDROMs

Oosterho PTh Bull Astron Inst Netherl

Walton ML Popular Astron

Williams M An Investigation of the Cepheid Variable Stars in the Scutum Cloud

PhD Dissertation Univ of Michigan Ann Arb or

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

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Octob er

HU ISSN

LIGHT CURVES FOR NOVA Mus AND NOVA Oph

1 2

WILLIAM LILLER ALBERT JONES

1

Instituto Isaac Newton Casilla Re nacaChile email wlillercompuservecom

2

Carter Observatory Ranui Road Stoke Nelson New Zealand email afjonesvoyagerconz

In an earlier Bulletin Liller Jones we describ ed and discussed light curves for

Nova Sgr and Nova Sco Here we consider the light curves of the two other

known galactic novae of that year Nova Mus and Nova Oph As b efore Jones made

visual observations while Liller used b oth photography and a CCD with a minusIR

lter a combination that results in a broadband V system extending from ab out nm

to nm and thus includes the H line

Nova Oph was discovered by Takamizawa on TMax lm on June and

Nova Mus was found by Liller a on Technical Pan lm taken through an orange lter

on Dec The light curves shown in Figures and are similar in that b oth show

a relatively smo oth steady decline Because of the very rapid fading of Nova Oph p o or

weather in New Zealand and a brief hiatus of observations in Chile we have augmented

Fig with additional V magnitudes rep orted by Hanzl

As for N Mus a casual rep ort by Seronik establishes that N Mus was pho

tographed by OMeara two nights b efore the nova was rst sp otted The star itself

app ears somewhat brighter than the discovery image From the print of OMearas

color photograph one would estimate a magnitude of  shown in Fig as a tri

angle at JD Using this observation we estimate that for Nova Mus t 

3

days for the visual observations and  days from the broadband V measurements

This dierence and the clear separation of the two light curves starting a few days after

discovery can b e understo o d from the diering resp onse of the two detectors to H the

broadband V lter is near p eak sensitivity at that wavelength whereas the eye resp onds

only weakly to H Indeed a sp ectrum taken of Nova Mus the day after discovery showed

H to b e exceptionally bright  times brighter than the neighboring continuum

Liller b Because the strength of H relative to the neighboring continuum in

creases steadily after the nova brightness has p eaked the visual observations would b e

exp ected to show a slower rate of decline Perhaps puzzling is the coming together of

the broadband V and the visual observations after ab out JD The cause may b e

the presence of a faint star or stars at or near the p osition of the nova which biased the

visual magnitude estimates or it may just b e that at this level of brightness the visual

magnitudes are systematically to o bright

For Nova Oph we estimate from Fig that t  days for Hanzls V magnitudes and

3

 days for the visual observations Again this dierence can b e understo o d from

the diering resp onse to H the standard V lter is designed blo ck the light from this

IBVS

Figure Light curves of Nova Mus showing Jones visual estimates as lled circles and Lillers

broadband V magnitudes as plus signs The triangle shows the approximate values derived from

OMearas prediscovery color photograph Two photographic magnitudes by Liller are indicated by a

lled circle with rays from the discovery photograph and by a v denoting a fainterthan

prediscovery observation

Figure Light curves of Nova Oph showing Jones visual estimates as lled circles and Hanzls

CCDV magnitudes as plus signs Takamizawas photographic discovery is indicated with a lled circle

with rays and two unpublished photographic magnitudes by Liller show as a triangle and as a v denoting a fainterthan prediscovery observation

IBVS

strong emission whereas the eye retains some sensitivity at that wavelength Filipp enko

et al rep orted that CCD sp ectra of Nova Oph showed strong emission lines of

H and their note implies that H was the strongest line recorded

As usual uncertainty in the values of t arises from the imp erfectly known time and

3

magnitude when p eak brightness was reached We note that for N Oph days elapsed

b etween the discovery date and the preceding patrol of the area while for N Mus the

interval b etween when OMearas photograph was taken and the preceding negative ob

servation of the area was days

Finally we reiterate the conclusion reached in our earlier rep ort Liller Jones

namely that although classically the value of t should b e evaluated using bluesensitive

3

photographic emulsions the values derived from visual observations should agree quite

well with the classical values and they are certainly sup erior in this regard to standard

V observations

We again wish to thank Drs Nikolai Samus and Hilmar Duerb eck for their interest

and for encouraging us to publish our nova light curves

References

Filipp enko AV Leonard DC Mo djas M Eastman RG IAU Circ No

Hanzl D IAU Circ Nos and

Liller W a IAU Circ No

Liller W b IAU Circ No

Liller W Jones AF IBVS No

Seronik G Sky Tel

Takamizawa K IAU Circ No

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

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A NEW Dor CANDIDATE IN CRUX

T ARENTOFT AND C STERKEN

Vrije Universiteit Brussel VUB Pleinlaan B Brussel Belgium

email tarentofvubacbe csterkenvubacbe

In January and March the Dutch cm telescop e at ESO La Silla was used for

uv by CCD observations of the WolfRayet star WR The observations were carried out

with a few data p oints each night during nights distributed over three observing runs

During the data reduction pro cess we found that one of the other stars in the eld showed

variability This star is not listed as variable in SIMBAD or in the GCVS Kholop ov

et al including the subsequent namelists Kholop ov et al

Kazarovets Samus Kazarovets et al The observed eld is

shown in Figure where the new variable star is marked by an arrow Its co ordinates

h m s  0 00

are and A light curve from March is shown

in Figure together with the dierence b etween the comparison stars The overall r ms

scatter in the comparison star light curve is ab out mmag

Figure CCD frame covering the region where the new variable has b een found arrow The bright

0

star : north of the new variable is WR

IBVS

At least two of the nights had photometric conditions We used the star HD

in the nearby Car region to determine the zerop oint shift to the standard system

using the photometry of Kaltcheva Georgiev The average colour indices with

estimated errors are

y 

b y 

m 

c 

The errors on the observed indices are rather large mainly due to observational noise

but also due to the variability of this faint ob ject The Stromgren colour indices are

consistent with a late A or early F star

Figure Light curve of the new variable Crosses are the variable minus the average of two

comparison stars diamonds the dierence b etween the two comparison stars with shifted zerop oint

Fourier analysis of the y light curve reveals the presence of two frequencies The

h m s

rst is at Hz cd corresp onding to a p erio d of and with a

semiamplitude of mmag The second has a frequency of Hz cd

h m s

P and a semiamplitude of mmag No excess p ower is left in the

amplitude sp ectrum after these two frequencies have b een subtracted from the light curve

The noise level at low frequencies in the residual sp ectrum is ab out mmag No p eaks

higher than ab out mmag are present in the amplitude sp ectrum of the comparison stars

The sp ectral class the multiperio dicity and the p erio ds and amplitudes of the variations

lead us to suggest that we are dealing with a variable star of the Doradus class

Doradus variables are a new class of pulsating stars consisting of nonradial g mo de

pulsators with p erio ds b etween hours and ab out three days In the HR diagram they

cluster around the intersection of the red edge of the classical instability strip with the

IBVS

main sequence Handler Fig is the observational HR diagram for the Dor

stars for which uv by photometry is available with b y and M determined by the

V

metho d of Mo on Dworetsky All known Dor stars have with

an average  Using these limits for the reddeningfree index we obtain

for the new variable average b y  M  and T  K

V e

leading to the p osition in the HR diagram shown by the op en symbol

1

2 V M

3

0.15 0.20 0.25

(b-y)0

Figure Observational HR diagram lled symbols are the p ositions for known Doradus stars

the op en symbol denotes the lo cation of the new Dor candidate The error bars reect the

uncertainty due to the exp ected range The full line is the ZAMS line given by Crawford the

dotted lines are the empirical b orders of the Dor lo cus as given by Handler

 a measure of blanketing Our colour indices also yield a surprisingly high

m

0

for a given that correlates well with metallicity FeH the largest p ositive value

m

0

known for Dor stars

TA and CS acknowledge nancial supp ort from the Belgian Fund for Scientic Re

search FWO This research has made use of the SIMBAD database op erated at CDS

Strasb ourg France and the NASA Astrophysics Data System

IBVS

References

Crawford D L AJ

Crawford D L Mandwewala N PASP

Handler G MNRAS in press

Kaltcheva N T Georgiev L N MNRAS

Kazarovets E V Samus N N IBVS No

Kazarovets E V Samus N N Goranskij V P IBVS No

Kazarovets E V Samus N N IBVS No

Kazarovets E V Samus N N IBVS No

Kholop ov P N et al General Cat of Var Stars th ed Nauka Moscow

Kholop ov P N et al IBVS No

Kholop ov P N et al IBVS No

Kholop ov P N et al IBVS No

Mo on T T Dworetsky M M MNRAS

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

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CCD OBSERVATION OF THE NOVEMBER OUTBURST OF V Peg

AN SU UMaTYPE DWARF NOVA WITH A LONG ORBITAL PERIOD

T KATO K MATSUMOTO

Dept of Astronomy Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp katsurakusastrokyotouacjp

V Peg is a dwarf nova discovered during the sup ernova survey at the Beijing As

tronomical Observatory Qiu et al a Qiu et al b rep orted another bright

outburst at R on November UT The rep orted amplitude exceeding

1

mag and the rapid decline mag d rate at the time of make the ob ject a go o d

candidate for an SU UMatype dwarf nova Kato During this bright outburst we

observed the variable in order to detect p ossible sup erhumps

2

2.5

3 Relative magnitude

3.5

1.88 1.9 1.92 1.94 1.96 1.98 2 2.02 2.04

HJD - 2450770

Figure Light curve of V Peg

IBVS

The observations were done on November using an unltered ST camera

attached to the Meade cm SchmidtCassegrain telescop e The exp osure time was

s The images were darksubtracted atelded and analyzed using a micro computer

based ap erture photometry package developed by one of the authors TK The ux of

the variable was measured relative to GSC USNO r magnitude whose

constancy was conrmed by comparison with GSC USNO r magnitude

The magnitudes given b elow are expressed relative to GSC

Figure illustrates the light curve of the present observation Although the run was not

long enough to conrm the p erio dicity there was a humplike feature with an amplitude

of mag around HJD We consider this is a sup erhump by taking into

account the considerable duration of the outburst the ob ject was still in outburst on

Dec at mag by L T Jensen the brightness of the outburst and the usual lack of

mo dulations of this amplitude in SS Cygtype dwarf novae The sup erhump p erio d seems

to b e longer than hours as the length of the observation was  hours Although this

p erio dicity should b e conrmed by future observations the p otential p erio d makes V

Peg as a candidate of the longest orbitalp erio d SU UMatype dwarf novae cf Nogami et

al or even may b e the second dwarf nova in the p erio d gap Nogami et al

Future monitoring of outbursts and intensive timeresolved photometry are needed

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture and Sp orts TK Part of this

work is supp orted by a Research Fellowship of the Japan So ciety for the Promotion of

Science for Young Scientists KM

References

Kato T vsnetalert circulation No

httpwwwkusastrokyotouacjpvsnetMailvsnetalertmsghtml

Nogami D Masuda S Kato T PASP

Nogami D Kato T Baba H Masuda S PASJ L

Qiu YL Qiao Q Y Hu JY Esamdin A a IAUC No

Qiu YL Qiao Q Y Hu JY Esamdin A b IAUC No

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

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HU ISSN

PREOUTBURST ACTIVITY OF V Sgr SAX J

POSSIBLE EXISTENCE OF DAY PERIOD

1 1 2 3 4

T KATO M UEMURA R STUBBINGS T WATANABE B MONARD

1

Dept of Astronomy Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp uemurakusastrokyotouacjp

2

Greenland Drive Drouin Victoria Australia email stubb oqedsystemscomau

3

VSOLJ Shirao dormitory Oonakazato Shizuoka Japan email jccniftynejp

4

PO Box Die Wilgers Pretoria South Africa email LAGMonarcsircoza

Goranskij discovered an eruptive variable star in the close vicinity of the

nominal p osition of Luytens variable HV Goranskijs ob ject once to ok over the

GCVS nomenclature GM Sgr of HV However recent studies Morel Hazen

suggest they are two indep endent variables We use the new GCVS designation of

V Sgr Samus for Goranskijs ob ject throughout this pap er Readers please

pay sp ecial attention b ecause several references already list the Xray transient as GM

Sgr Goranskij rep orted a single short outburst in recorded on Moscow

photographic plates reaching B Goranskij also suggested the p ossible

presence of a p erio dicity of day from the analysis of the quiescent data

V Sgr b egan receiving attention since this star was prop osed as the p ossible optical

counterpart of the faint aring Xray transient SAX J in t Zand and Heise

based on the p ositional coincidence The optical b ehavior of V Sgr however

was rather overlooked until the discovery of a new optical outburst in August

Watanabe After a p erio d of apparently increasing activity the ob ject went into a

giant optical outburst reaching m on September Stubbings which

V

was followed by an intense Xray are Smith et al

In this pap er we rep ort on the unusual optical activity prior this giant optical and X

ray outburst The CCD observations were done using an unltered ST camera attached

to a cm SchmidtCassegrain telescop e at Kyoto University The exp osure time was

TM

s The images were darksubtracted atelded and analyzed using the Java based

ap erture photometry package developed by one of the authors TK The magnitudes of

V Sgr were determined using the GSC Tycho V B V

whose constancy was conrmed by comparison with GSC The estimated R

C

magnitude was used to calculate unltered CCD magnitudes of V Sgr The small

dierence of the rep orted color of V Sgr Goranskij and that of the comparison

will make unltered CCD magnitudes a go o d approximation of R magnitude of the

C

variable Visual observations were made using cm telescop es by Stubbings Watanabe

and Monard All visual observations used the V magnitude sequences The comparison of

quasisimultaneous visual and CCD observations has conrmed the consistency b etween

IBVS

8

9

10

11

Magnitude 12

13

14

400 405 410 415 420 425 430 435 440

JD - 2451000

Figure Light curve of V Sgr

8

9

10

11

Magnitude 12

13

14

430 432 434 436 438 440

JD - 2451000

Figure Enlarged light curve of V Sgr showing quasip erio dic mo dulation prior to the giant outburst

IBVS

visual and CCD measurements The estimated error mag of visual estimates

do es not aect the following discussion

Figure represents the summary of present observation including the later giant out

burst for clarity Filled and op en circles represent CCD and visual observation resp ec

tively Some visual observations rep orted to VSNET have b een supplemented for con

structing the fading part of the outburst V Sgr rose gradually since the detection

by Watanabe The most remarkable feature was the presence of highamplitude

mo dulation Figure since JD six days b efore the giant outburst The mo d

ulation had an amplitude of  mag with a quasip erio d of days This p erio dicity

do es not t any of candidate p erio ds by Goranskij The observed p erio dicity can

b e either interpreted as arising from the mo dulation of the source activity or as reecting

the underlying binary p erio d Since the examination of the RXTE monitoring of the

galacticcenter region has revealed that the Xray from V Sgr was already detected

for this preoutburst p erio d Markwardt et al the optical mo dulation may have

caused by the reection eect by the Xray heating on the secondary In this interpre

tation the day p erio d corresp onds to the orbital p erio d which awaits conrmation

by future radial velocity studies Otherwise the cause of previously unrecorded recurrent

quasip erio dic brightening should b e sought

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture and Sp orts TK

References

Goranskij V P Astron Tsirk No

Goranskij V P IBVS No

Hazen M vsnetchat circulation No

httpwwwkusastrokyotouacjpvsnetMailvsnetchatmsghtml

in t Zand J Heise J IAUC No

Markwardt C B Swank J H Morgan E H IAUC No

Morel M vsnetchat circulation No

httpwwwkusastrokyotouacjpvsnetMailvsnetchatmsghtml

Samus N N IAUC No

Smith D A Levine A M Morgan E H IAUC No

Stubbings R IAUC No

Watanabe T VSOLJ Variable Star Bul letin

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

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Octob er

HU ISSN

NEW ELEMENTS AND LIGHT CURVE OF CR TAURI

BAV MITTEILUNGEN NO

FRANZ AGERER

Bundesdeutsche Arb eitsgemeinschaft f urVeranderliche Sterne eV BAV Munsterdamm D Berlin

Germany

Name of the ob ject

CR Tau S Tau

Observatory and telescop e

Private Observatory cm SCT

Detector SBIG ST camera

Filters None

Comparison stars GSC

Check stars GSC

Transformed to a standard system No

Remarks

CR Tau was discovered by Homeister a photographic minima were used

to derive the rst elements Homeister b These elements are listed in the

GCVS Recently we could observe photo electrically ten new minima which showed

the GCVSephemeris to b e a spurious one The minimum times are calculated ac

cording to the Kweevan Woerden metho d Using all available photo electric

minima a weighted least squares t led to the new ephemeris

d

Min I HJD  E

 

Acknowledgements

Data from the Lichtenknecker Database were used

IBVS

Table Observed times of minima for CR Tau ep o chs and residuals computed with resp ect to the

linear ephemeris derived in this pap er

JD hel JD hel

 

Type Ep o ch O C Ref Type Ep o ch O C Ref

P P

P E

P E

P E

P E

P E

E P

P E

P E

P E

P E

P E

P E

P



P denotes photographic minima weight and E CCD observed minima weight

Those marked with got reduced weight

Homeister b Agerer this pap er Diethelm Diethelm

Figure Dierential light curve of CR Tau drawn with the new ephemeris

References

Diethelm R BBSAG Bul letin

Diethelm R BBSAG Bul letin

Homeister C a Erg AN

Homeister C b VSS

Kholop ov P N et al General Catalogue of Variable Stars th Edition Nauka

Moscow

Kwee K K van Woerden H Bul l Astr Inst Netherlands

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

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DIFFERENTIAL PHOTOMETRY

OF SUSPECTED CATACLYSMIC VARIABLES

N BENNERT I KONIG E MANTHEY H BLEUL K FIEGER M HESS A HOVEST

;

W HOVEST T JURGES J KLEIMANN C KRIEGESKORTE E KRUSCH

;

D MUNSTERMANN D REYMANN K ROSLER M NIELBOCK M POHLEN

; ;

L SCHMIDTOBREICK C TAPPERT R VANSCHEIDT

1

Astronomisches Institut RuhrUniversitatBo chum Universitatsstrae D Bo chum Germany

email hlist usersastroruhrunibochumde

2

UniversitatDortmund OttoHahnStrae D Dortmund Germany

3

Osservatorio Astronomico di Padova Viccolo dellOsservatorio I Padova Italy

4

UniversitatHeidelb erg Alb ertUb erleStrae D Heidelb erg Germany

5

S udring D Warendorf Germany

We here present dierential photometry of the four susp ected cataclysmic variables

CVs HM Aur FBS FBS and NSV and of the three known

CVs HQ And RX And and FO Per The target ob jects were selected from the CV cat

alogue of Downes et al hereafter DWS searching for not yet conrmed CVs

and p o orly observed systems with unknown orbital p erio ds Therefore the list of Ritter

Kolb was used to exclude ob jects with known p erio ds To evaluate the signicance

of our results we included three systems with a certain CV classication

The data were taken at Hoher List Observatory on March and on Octob er

and on March in the framework of the Astronomisches Beobachtungsprak

tikum of the RuhrUniversitatBo chum We used an astrograph D m f m

and a Cassegrain reector D m f m equipp ed with Ford Loral FA

CCDs and Johnson Vlters In order to resolve the CVtypical shortterm variation

ickering the integration time was limited to sec thus constraining the accessible

Vmagnitude to Table lists the details of the observations

Standard reduction was p erformed with IRAF packages using overscan and dome

or skyats for the m telescop e biasframes and skyats for the astrograph data

Ap erture photometry was done with the DAOPHOT package On each image frame we

chose all nonsaturated comparison stars comprising a SNratio greater or equal to the

SNratio of the target ob ject For j n let I t denote the instrumental intensity

j

j

t of comparison star j at time t For t t t all dierential lightcurves I

b egin end

k

I t I t j k f ng j k were calculated For t t t the average

j k b egin end

lightcurve I t was computed as the arithmetic mean of all comparison star intensities

av

j

Then dierential magnitudes were calculated according to I t I t I t All

j av

av

comparison stars with brightness variations ab ove the noise level were easily discriminated

1 IRAF is distributed by the National Optical Astronomy Observatories

IBVS

Table List of observations The co ordinates in columns and have b een taken from DWS

Column shows the instrument used while columns and give the number of data p oints lightcurves

of observations marked with a have b een omitted in this pap er and the total time coverage p er night

resp ectively

Ob ject RA DEC Instrument Date n t h

data obs

HM Aur astrograph

FBS m telescop e

FBS m telescop e

NSV astrograph

HQ And m telescop e

RX And astrograph

FO Per m telescop e

and subsequently excluded from the average lightcurve In an iterative pro cess only

comparison stars with constant brightness within the noise level contributed to the average

lightcurve

HM Aur This system has b een discovered by Geyer et al who describ ed it as a

longp erio d variable showing irregular waves spanning over days with an amplitude

of mag However Vogt susp ected a quiescent nova while DWS list it as

novalike with photographic magnitudes To our knowledge no sp ectrum has

b een published

FBS and FBS Both ob jects have b een rep orted as p ossible

CVs by Abramyan Mikaelyan as discoveries of the First Byurakan Ob jec

tive Prism Survey The authors do not present nding charts Therefore charts published

by DWS are based on the published co ordinates only The rep orted magnitudes are

V for FBS and B for FBS resp ectively While for

FBS a sp ectrum is not available FBS has recently b een studied by

Liu et al who classied it as a DAB type white dwarf

NSV NSV is listed in the NSV catalogue of Kholop ov as a p ossible

dwarf nova No sp ectrum has b een published so far and therefore this classication

remains uncertain DWS give a magnitude range of V

HQ And HQ And is listed as a CV in DWS with a magnitude range of m

phot

Meinunger rst classied HQ And as a rapid irregular star and revised

it later in favour of a CV classication She already susp ected a p ossible p olar

nature which was subsequently strengthened by the p olarimetry of Andronov Meinunger

RX And RX And is a wellknown dwarf nova of subtype Z Cam with a magnitude

range of V DWS Sp ectroscopic studies were conducted eg by Kaitchuck

et al and Smith et al while Verbunt et al present a lightcurve

The orbital p erio d has b een determined to P hours by Kaitchuck

FO Per According to Howarth and Gessner FO Per is a dwarf nova

with a mean outburst cycle length of roughly days The sp ectrum published by Bruch

shows the typical strong emission lines of such a system and thus supp orts this

classication DWS give a maximum visual magnitude of and a photographically

IBVS

Table Results of the dierential photometry are given in this table Column shows the average

magnitude of the dierential lightcurve for the target and the comparison stars CSCS Comparison

stars marked with a are used to calculate the average lightcurve

HJD Ob ject V HJD Ob ject V

di di

HM Aur  NSV 

 

CS CS 



CS  CS 

CS  NSV 



CS  CS 



HM Aur  CS 



CS

CS 

CS 

CS 

HJD Ob ject V

di

HM Aur 



CS

HQ And 



CS 

CS 



CS 

CS 

CS 

CS 



CS 

FBS 



CS 

CS 



CS 

CS 



CS

RX And 



FBS 

CS 



CS 

CS 

CS 

FO Per 



CS

CS 



FBS 

CS 





CS 

CS 



CS 

CS 



CS 

CS 



CS 

CS 

determined minimum value of

In Table we give the mean dierential magnitudes together with their standard

deviation over the night Figure shows the lightcurves of the program stars as plots

of the dierential magnitude except for FO Per and RX And where the calibrated V

magnitude was available against time in units of the Helio centric Julian Date HJD All

magnitudeaxes cover a range of mag while all HJDaxes cover a time of d thus

rendering all lightcurves directly comparable The nding charts on the left side of Figure

give the lo cation of the ob jects as well as of all comparison stars referred to in Table

for which dierential lightcurves were computed

Known CVs HQ And RX And and FO Per

It is evident from Table that the standard deviation of the dierential lightcurve is

much higher than those of the comparison stars The dierential lightcurves of HQ And

and RX And show the characteristic ickering while the lightcurve of FO Per shows a slow

descent Furthermore we can derive a calibrated magnitude for FO Per and RX And as

several comparison stars have b een measured as secondary standards by Misselt

IBVS

HQ And

RX And

FO Per

Figure On the left side we present the nding charts for the analyzed stars On the right side the

corresp onding lightcurves Magnitude vs HJD are displayed Scales were chosen to b e directly

0 0 0 0

comparable Finding charts HM Aur dimensions  FBS  FBS

0 0 0 0 0 0 0 0 0 0

 NSV  HQ And  RX And  and FO Per  North is up

East is to the left Numbers corresp ond to the comparison stars

IBVS

HM Aur

FBS

FBS

NSV

Figure cont

IBVS

For RX And we thus obtain a visual magnitude of V and for FO Per

V The latter value lies almost exactly in the middle of the ab ove

mentioned magnitude range We therefore conclude that our observation must have taken

place shortly after an outburst while the CV was still in its decline

Candidate CVs HM Aur FBS FBS and NSV

In the cases of HM Aur FBS and NSV the resulting lightcurves show a

straight line at a constant magnitude None of the targets shows a standard deviation

signicantly higher than those of the comparison stars Furthermore all ob jects which

could b e observed in more than one night always show the same average magnitudes within

the errors We therefore conclude that a CV nature seems unlikely for these ob jects As

for FBS due to the large uncertainties and the short time interval we do not

consider our lightcurve to provide sucient information to sp eak in favour or against a CV

classication However the very recently published sp ectrum by Liu et al clearly

lacks any CV characteristic We thus take the fact that the most doubtful lightcurve was

obtained from an ob ject which was proven afterwards not to b e a CV to strengthen our

conclusions on the other three candidates although sp ectroscopic observations will b e

required to nally clarify their status

Acknowledgements We thank the director of the Hoher List Observatory Prof Dr

W Seggewiss for generous allo cation of observing time

References

Abramyan HV Mikaelyan AM Astrophys

Abramyan HV Mikaelyan AM Astrophys

Andronov IL Meinunger L IBVS

Bruch A AAS

Downes R Webbink RF Shara MM PASP DWS

Gessner H Mitt VerandSterne

Geyer E Kipp enhahn R Strohmeier W Kleine VeroBamberg

Howarth ID Mitt VerandSterne

Kaitchuck RH Mansp erger CS Hantzios PA ApJ

Kaitchuck RH PASP

Kholop ov P ed New catalogue of variable stars Moscow Publ Oce Nauka

Liu W Hu JY Li ZY Cao L ApJS

Meinunger L Mitt VerandSterne

Meinunger L IBVS

Misselt KA PASP

Ritter H Kolb U AAS

Smith D Mateo M Szkody P Astrophys Space Sci

Verbunt F Pringle JE Wade RA et al MNRAS

Vogt N in Classical Novae Bo de MF Evans A eds Wiley Sons p

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

Octob er

HU ISSN

NEW VARIABLE STARS DISCOVERED IN THE MISAO PROJECT

IV MisVMisV

SEI ICHI YOSHIDA KENICHI KADOTA TAICHI KATO

1

MISAO Pro ject Miyawada Fujishiromachi Kitasomagun Ibaraki Japan

email seiichimuraokainfowasedaacjp

2

MISAO Pro ject Koshikiya Ageo City Saitama Japan

email kenickastroartscojp

3

Dept of Astronomy Kyoto University Kyoto Japan email tkatokusastrokyotouacjp

This rep ort describ es new variable stars MisVMisV discovered in the

course of the MISAO Pro ject

These ob jects are detected automatically by the PIXY system as candidates of variable

stars from unltered CCD images taken by Kadota b etween April and July and a

few in November then conrmed by Yoshida and Kadota Further details are same

as describ ed in Yoshida and Kadota

Table lists new variable stars The p ositions and magnitudes were measured using

USNOA catalog The magnitude is based on a preliminary V magnitude calculated

from R and B magnitude in the catalog based on Katos equation

V R B R

The nding charts are available electronically as fnnneps where nnn refers to the

serial number assigned to the star in the rst column of Table

V Cyg is arcmin from MisV that was detected on our unltered CCD

image as a mag star MisV is thus another new variable star

BL Sct is arcmin from MisV No star brighter than mag was detected at

the p osition of BL Sct on our unltered CCD images on Apr and May However

considering the large angular distance MisV is probably another variable ob ject

NSV is arcmin from MisV No star brighter than mag was detected

at the p osition of NSV on Apr and July Therefore MisV may b e

identied with NSV

NSV is arcmin from MisV that was detected on our unltered CCD

image as a mag star Therefore MisV is another new variable star

NSV is arcmin from MisV that was detected on our unltered CCD

image It was fainter than mag on Apr but mag on July Therefore

MisV is another new variable star

IBVS

Table List of New Variable Stars

Unltered

Co de RA J Decl CCD Mag Type Identied with

Max Min

h m s  0 00

MisV : : USNOA

IRAS

MisV USNOA

IRAS

MisV IRAS

MisV USNOA

IRAS

MisV IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV IRAS

MisV IRAS

MisV IRAS

MisV IRAS

MisV USNOA

IRAS

MisV IRAS

MisV USNOA

IRAS

MisV IRAS

MisV IRAS

MisV IRAS

MisV IRAS

MisV USNOA

IRAS

MisV IRAS

MisV USNOA

IRAS

MisV IRAS

MisV IRAS

MisV IRAS

MisV IRAS

MisV USNOA

IRAS

MisV IRAS

MisV IRAS

MisV USNOA

IRAS

MisV GSC

USNOA IRAS

IBVS

Table cont

Unltered

CCD Mag

Co de RA J Decl Type Identied with

Max Min

h m s  0 00

MisV : : IRAS

MisV IRAS

MisV USNOA

IRAS

MisV GSC

USNOA

MisV SR USNOA

MisV USNOA

MisV

MisV SR GSC

USNOA

MisV SR USNOA

MisV USNOA

MisV IRAS

MisV USNOA

MisV USNOA

MisV GSC

USNOA

MisV USNOA

MisV

MisV IRAS

MisV SR IRAS

MisV M IRAS

MisV SR USNOA

IRAS

References

Yoshida S Kadota K IBVS No

Kato T httpwwwkusastrokyotouacjpvsnetMailvsnetchatmsghtml

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

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Octob er

HU ISSN

VARIATIONS IN THE EFFECTIVE TEMPERATURE

AND THE BALMER JUMP OF THE Ap STAR Tauri

NA SOKOLOV

Central Astronomical Observatory at Pulkovo St Petersburg Russia email sokolovgaospbru

The magnetic ApSi star Tau GS Tau Bp Si was found to b e variable by

Rakos with a p erio d of around days Blanco and Catalano also conrmed

this p erio dicity Subsequently Abt and Snowden discovered the sp ectroscopic bi

d

narity of Tau and determined an orbital p erio d of a value also adopted by

Wol The investigation of the visible sp ectrum by Wol established the syn

chronism b etween rotation and revolution for this star Moreover Wol recorded

Zeeman sp ectrograms of this star and determined the variations of the eective magnetic

eld suggesting a maximum near phase These sp ectrograms also yielded variations

of Si I I Sr I I and Ti I I lines and showed that the Si I I minimum near phase coincides

approximately with the maximum brightness whereas Sr I I and Ti I I minima o ccur near

phase Moreover Artru and FreireFerrero who observed Tau with the IUE

satellite conrmed the results of Wol They showed that the minimum of silicon

absorption o ccurs at phase just b efore the gallium maximum at phase More

recently Gonzalez and Artru used the visible sp ectra to derive variations of the O I

lines at and A and found that there must b e an accumulation

of oxygen around the p ositive magnetic p ole of Tau

A new metho d of determination of the eective temp erature T of the chemically

e

p eculiar stars using the Balmer continuum slop e near the Balmer jump was prop osed by

Sokolov Using this metho d it is p ossible to measure the size of the Balmer jump

D as well see Sokolov To check the reliability of this metho d the star Tau

was selected b ecause there is evidence for variability in the size of the Balmer jump

for this star Adelman Fourteen continuum energy distributions in the sp ectra of

Tau were taken from the pap er Adelman The scans have seven measurements

in the Balmer continuum that allowed to calculate the T from the slop e of sp ectra in the

e

Balmer continuum with reasonable accuracy To determine the continuum shap e at b oth

sides of the Balmer jump an iterative pro cedure was used The Balmer jumps of Tau

were calculated by extrap olating the two tted curves to A as describ ed by

Sokolov The errors on eective temp eratures and on size of the Balmer jumps

were computed according to the formula for the standard error propagation theory The

phases for the observational data in our investigation were computed using the ephemeris

adopted by Abt and Snowden

The variations in the eective temp erature and Balmer jump of Tau are plotted on

the middle and b ottom panels of Fig resp ectively As one can see from Fig b oth

IBVS

T and D reveal clear variation with phase for Tau Although the statistical error of

e

the T determinations for individual scans is large enough up to K In order to nd

e

the amplitude of the T and D variations a linearized leastsquares metho d was used

e

which was describ ed by North A leastsquares t by onefrequency cosine curve

was applied b oth to the T and to the D variations The tted curves are plotted as

e

the solid lines in Fig The computations give the minimum of the T K and

e

D dex at the phases and resp ectively Also the maximum of the T

e

K is at phase and is consistent with the maximum of D dex at phase

Figure The variations in the b y color index eective temp erature and Balmer jump for Tau

The top panel shows the b y color index variations observed by Wol lled circles and

synthesized from sp ectrophotometry by Adelman op en circle s The middle panel shows the

eective temp erature variations The b ottom panel displays the Balmer jump variations The solid lines are least squares t

IBVS

It is wellknown that the u b and b y color indices of Stromgrenphotometry mea

sures the size of the Balmer jump and the slop e of the Paschen continuum resp ectively

Adelman established the changes in the size of the Balmer jump from the u b

index variations and two scan comparisons Moreover he noted that the b y index can

b e describ ed as constant although the values suggest low amplitude variability but the

slop e of the Balmer continuum is not quite correct

To test the validity of the obtained phase diagrams of the T and the D variations

e

the u b and b y indices were used The correlation b etween the D and the u b

index variations is excellent as is illustrated by Fig and by Fig from the pap er by

Adelman It should b e noted that the minimum of D corresp onds to the maximum

of the light b oth in the Paschen continuum and in the Balmer continuum see Wol

The slop e of the Paschen continuum is a go o d estimator of T for hot CP stars in the

e

visual sp ectral region To investigate the correlation b etween variations of the slop e of

the Paschen continuum and the variations of T derived from the slop e in the Balmer

e

continuum the b y color index was used The top panel of Fig shows the b y index

variations of Tau The solid line is a least squares t by a onefrequency cosine curve

The tted curve conrms the low amplitude variability of the b y color index for this star

although the scattering of the p oints in the top panel of Fig is large The correlation

b etween the slop e in the Paschen continuum and the T derived from the slop e in the

e

Balmer continuum variations app ears to b e very go o d as is illustrated by Fig The

minimum of the b y index is at phase and is consistent with the minimum of the

T This supp orts the reliability of the obtained phase diagram for the T variations

e e

On the other hand the minimum of the T corresp onds to the maximum light Moreover

e

the observations of Tau show that Si minimum coincides with maximum light at the

phase Wol However Mantegazza et al found that the shap e of the

light curve of Tau is variable on the timescale of a few years

In conclusion the present analysis of Tau shows that the metho d prop osed by

Sokolov is of sucient accuracy to study the eective temp erature and the Balmer

jump variations with phase for Ap stars

This work has b een supp orted by the Russian National Foundation for Astronomy

pro ject No The author wishes to thank the referee DM Pyp er for her helpful

comments which improved the pap er

References

Abt HA Snowden MS Astrophys J Suppl Ser

Adelman SJ Astron Astrophys Suppl Ser

Artru MC FreireFerrero R Astron Astrophys

Blanco C Catalano FA Astron J

Gonzalez JF Artru MC Astron Astrophys

Mantegazza L Poretti E Rib oni E IBVS No

North P Astron Astrophys Suppl Ser

Rakos KD Lowell Obs Bul l

Sokolov NA Astron Astrophys Suppl Ser

Sokolov NA Astron Astrophys Suppl Ser

Wol SC Astrophys J

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

NEW ANALYSES OF V CYGNI LIGHT CURVES

1 2 2 2

CLAUD H LACY MAMNUN ZAKIROV GC ARZUMANYANTS NR BAIRAMOV

2

AS HOJAEV

1

Department of Physics University of Arkansas Fayetteville AR USA

2

High Altitude Maidanak Observatory Astronomical Institute Tashkent Uzb ekistan

Lacy reanalyzed the photometry of G ulmen et al and combined the

results with his sp ectroscopic orbit to determine the absolute prop erties of this triple star

He found anomalies in the absolute prop erties of this system The primary comp onent

app eared to b e very small for its mass and the secondary app eared to b e less massive

but considerably larger than the primary which seemed to imply it might b e a premain

sequence ob ject A new set of B V light curves is now available for this system They

were obtained at the High Altitude Maidanak Observatory in Uzb ekistan with a m

reector Times of minima derived from these data have b een rep orted Lacy et al

From these times of minima and those of G ulmen et al we nd an improved

ephemeris Min I n where the uncertainty in the

last digits is shown in parentheses We have now t an orbit to these new data and nd

signicant dierences with the previous photometric orbit

The new data were analyzed with the NDE mo del Etzel Popper Etzel

as were the older data The results are presented in Table and shown in Fig and

Table Analyses of V Cyg Light Curves

G ulmenet al Data Maidanak Data

Parameter

B V B V

J    

s

r    

p

k    

i deg    

L    

A

L    

C

u

A

u

B

se mag

N

Note L L L

A B C

Some of the parameters are consistent across all analyses the orbital inclination i

and the third light L All other parameters dier signicantly The ratioofradii for

C instance is less than in the analysis of the newer data which would remove the anomalies

IBVS

found by Lacy Internally estimated uncertainties of the tted parameters are

comparable in b oth analyses although the residual standard errors se are smaller for

the light curves of G ulmenet al

Our conclusion is that the individual radii are much more p o orly known than are im

plied by the internal errors of the mo del ts Although the sumofradii is welldetermined

the ratioofradii is p o orly known A much more accurate set of light curves will b e needed

to denitively determine the radii of the comp onents of this binary star

Figure Light curve of G ulmenet al with tted orbit

Figure Light curve obtained at Maidanak Observatory and tted orbit

References

Lacy CHS AJ

Lacy CHS Clem JL Zakirov M Arzumanyants GC Bairamov NR Ho jaev

AS IBVS No

Etzel PB in Photometric and Sp ectroscopic Binary Systems ed EB Carling

Z Kopal NATO ASI Ser C Dordrecht Reidel

G ulmenO Sezer C G udur N AAS

Popper DM Etzel PB AJ

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

NSV IS A SHORT PERIOD VARIABLE IN OPHIUCHUS

1 2

ENRIQUE GARCIAMELENDO FLORENTINO SANCHEZBAJO

1

Esteve Duran Observatory El MontanyaSeva SEVA Barcelona Spain

email duranobsastrogeacescaes

2

Departamento de Electronica e IngenieraElectromecanicaEscuela de IngenierasIndustriales Universidad

de Extremadura Ctra de Elvas sn Bada joz Spain email fsanba jounexes

Name of the ob ject

NSV HV CSV GSC

Equatorial co ordinates Equinox

h m s  0 00

RA DEC

Observatory and telescop e

Esteve Duran Observatory m Cassegrain telescop e Extremadura University

Observatory m Newton telescop e

Detector CCD

Filters V

Comparison stars GSC

Check stars GSC GSC GSC

Transformed to a standard system No

Availability of the data

Up on request

Type of variability RRc

Remarks

PNSV was rst announced as a variable star by HughesBoyce and Huruhata

who indicated that this ob ject was an RR Lyr with a photographic magni

tude variation b etween and Our observations show that NSV is a

short p erio d variable with a very symmetric light curve probably of the RRc type

although we do not exclude the p ossibility of this ob ject b eing a binary system

The amplitude is magnitudes in the V band The following ephemeris has

b een computed

d

Max JD    E

IBVS

Figure

Reference

HughesBoyce E Huruhata M HA No

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

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November

HU ISSN

UBV PHOTOELECTRIC TIMES OF MINIMA OF THE

ECLIPSING VARIABLE TV CASSIOPEIAE

1;2 1;3 1

F FAGHIHI N RIAZI A DARIUSH

1

Biruni Obs Shiraz University Shiraz Iran email faghihiphyssuscacir

2

The Islamic Azad University of Firo ozabad Firo ozabad Iran

3

Physics Dept Shiraz University Shiraz Iran

TV Cas is a short p erio d semidetached eclipsing binary that consists of a nearly

spherical more massive BV star and a larger co oler and tidally distorted G IVI I I

comp onent whose surface is in contact with its Ro che lob e The orbital p erio d of TV Cas

is days de Landtsheer The orbital and physical prop erties of TV Cas

have b een determined by Khalesseh et al from the analysis of its light and radial

velocity curves

TV Cas was observed by us during and observing seasons with the cm

 0

Cassegrainian telescop e of the Biruni Observatory Latitude N Longitude

 0 00

E We used an unrefrigerated RCA photomultiplier tub e and the obser

vations were made through UBV lters which are closely matched to the standard UBV

 

system The comparison and the check stars were BD and BD resp ec

tively the same as used by Grauer et al

As is frequently the case for Algol systems the observations show evidence from phase

shifts of primary and secondary minima Figure shows the UBV light curves of TV Cas

where the phases were computed using the light elements of Grauer et al Also

the depths of the primary and secondary minima are given in Table

m

The probable errors of the individual observation were estimated to b e ab out in

m

the B and V lters and in the U lter These precision estimate were made from

an examination of the scatter in the outside eclipse p ortions of the light curves Table

contains observed minimum times cycle number and the O C values of the primary

minimum after recalculating the other available O C s rep orts according to Grauer et al

ephemeris Finally the O C curve is plotted in Figure

Our times of mideclipses were determined by making leastsquare parab olic ts to

the observations inside the eclipses The minimum times are the mean values of three

dierent lters the O C residuals were calculated using the ephemeris

d

Min I HJD  E

of Grauer et al A new ephemeris based on the recent timing is

d

Min I HJD  E

IBVS

-1.0

V -0.5

B

0.0

U

0.5 Delta Magnitudes

1.0

0.8 1.0 1.2 1.4 1.6 1.8

Phase Figure

0.06

0.05

0.04

0.03

0.02

0.01

0.00

-0.01

O-Cs (Days) -0.02

-0.03

-0.04

-0.05

-0.06 35000 40000 45000 50000

JD 2400000+ Figure

IBVS

Table The depth of minima according to the present study

Filter Min I Min I I

m m

U  

m m

B  

m m

V  

Table The photo electric times of primary minimum used in the O C curve

Hel JD O C

E Source

days

Huer Kopal

Huer Kopal

Huer Kopal

Chou

Lavrov

Bakos Tremko

Lavrov

Lavrov

Lavrov

Bakos Tremko

Friebo esConde Herczeg

Friebo esConde Herczeg

Friebo esConde Herczeg

Bakos Tremko

Bakos Tremko

Bakos Tremko

Bakos Tremko

Bakos Tremko

Friebo esConde Herczeg

Friebo esConde Herczeg

Friebo esConde Herczeg

Friebo esConde Herczeg

Papousek

Papousek

Papousek

Papousek

Papousek

Papousek

Grauer et al

Grauer et al

Grauer et al

Grauer et al

Grauer et al

Grauer et al

Grauer et al

Grauer et al

IBVS

Table cont

Hel JD O C

E Source

days

de Landtsheer

de Landtsheer

de Landtsheer

de Landtsheer

de Landtsheer

de Landtsheer

Borkovits Heged us

de Landtsheer

Margrave

de Landtsheer

de Landtsheer

de Landtsheer

Margrave

Wolf Diethelm

Wolf Diethelm

Present study

Present study

Present study

Present study

Grauer et al conclude that an approximate years p erio dicity exists in the O C

curve of TV Cas Our observations lend some supp ort to this idea

Acknowledgments Sincere thanks are due to Prof Edward F Guinan for his

guidance during th International School for Young Astronomers ISYA Zanjan Iran

References

Bakos GA Tremko J Bul l Astron Inst Czech

Borkovits T Heged us T Astron Astrophys Suppl

Chou KC Astron J

Friebo esConde H Herczeg T Astron Astrophys Suppl

Grauer AD McCall J Reaves LC Tribble TL Scott Shaw J Astron J

Huer CM Kopal Z Astrophys J

Khalesseh B Hill G Astron Astrophys

Landtsheer AC de IBVS No

Landtsheer AC de IBVS No

Landtsheer AC de Astron Astrophys Suppl

Lavrov MI Publ Stadt Astron Obs LeninStaatsuniv Kazan

Margrave TE IBVS No

Margrave TE IBVS No

Papousek J Bul l Astron Inst Czech

Wolf M Diethelm R IBVS No

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

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November

HU ISSN

THE PRECURSOR OF NOVA AQUILAE V Aql

1 1 1 2

D MORO U MUNARI T TOMOV A HENDEN

1

Padova and Asiago Astronomical Observatories I Asiago VI Italy

2

Universities Space Research Asso ciationU S Naval Observatory Flagsta Station P O Box Flagsta

AZ USA

Nova Aql V Aql was discovered in outburst by A Tago cf IAU Circ No

on July Detailed sp ectral observations by Tomov et al for the

days immediately following the maximum brightness set the expansion velocity of the

nova at  km sec note the strong NaI D interstellar lines which suggest a large

reddening and classify the nova among the Fe I I class of Williams

A detailed photometric monitoring of the nova evolution has b een provided by VSNET

It shows the nova reached a maximum brightness V  mag and has had a complex

decline over three months to V  mag

An imp ortant parameter for any nova is the identication of the precursor and con

sequently the measure of the outburst amplitude An accurate p osition for the nova

h m s  0 00

has b een provided indep endently by N James

J J

and G Masi cf IAU Circ No This corresp onds to an empty p osition b oth in DSS

00 00

and DSS with the closest stars at and distance as shown in Figure The cor

resp onding Palomar plates were taken on May and May resp ectively

The year time span is long enough to detect large prop er motions of the eld stars and

to extrap olate their p osition to the year The matching of the two plates do es not

reveal for any nearby star a prop er motion large enough to bring it to the p osition of the

nova for the ep o ch

The precursor of Nova Aql must have b een fainter than the plate limits for b oth

DSS and DSS which set the amplitude of the outburst in the m  mag range

However the precursor may have b ecome bright enough to show up on Schmidt patrol

plates if it underwent the smaller amplitude outbursts that characterize dwarf novae

DN A tight link b etween the binary system prop erties of DN and classical novae is

widely accepted in literature and there are classical novae for example GK Per Nova

Per that once back to quiescence conditions are showing DN outbursts cf Warner

This note describ es the results of our search for such DN outbursts of the precursor

of Nova Aql over some decades b efore the eruption by insp ection of archive plates

from the two Schmidt telescop es of the Padova and Asiago Astronomical Observatories

The two Schmidt telescop es and cm have collected more than

plates since In their plate archive we have found plates covering the eld of Nova

Aql The basic parameters for the plates are summarized in Table The limiting

magnitude of the plates has b een derived by comparison with a deep U B V RI comparison

sequence calibrated at USNOFS by one of us AH which will b e published elsewhere

IBVS

Figure Comparison of the same  arcsec region around the p osition of Nova Aql

indicated by the empty circle in the center from the Palomar DSS and DSS

The progenitor was to o faint in quiescence to b e recorded by the m Palomar

Schmidt and so it has b een for the smaller Asiago Schmidt telescop es Also no out

burst of the progenitor of Nova Aql has b een recorded on the Asiago plates whose

limiting magnitudes cluster around mag as shown in Table

There are two basic p ossibilities to account for the negative detection of DN outbursts

for the progenitor of the Nova Aql

 the progenitor did not exp erience DN outbursts in the decades preceding its eruption

as a classical nova

 the progenitor indeed went through DN outbursts but they have not b een recorded

on the patrol plates b ecause

they were of limited amplitude and the progenitor never b ecame bright enough

to b e recorded on the plates or

the DN outbursts of the progenitor were of normal amplitude but the progenitor

itself is so faint in quiescence that even at outburst maximum it is still to o faint

to b e recorded on the plates or nally

the outbursts are normal but rare and to ok place when we were not observing

With the data in hand it is not p ossible to distinguish among these dierent p ossibil

ities However it seems fair at least to conclude that the nova progenitor did not have

frequent outbursts of large amplitude

We have already p erformed a similar investigation for the precursor of Nova Cas

which was bright enough in quiescence to b e easily recorded by the Asiago patrol plates

Munari et al As in the current study of Nova Aql the search for DN

outbursts in Nova Cas b efore its eruption as a classical nova gave negative results

IBVS

Table Schmidt plates from the Asiago archive containing the eld of Nova Aql The last column

gives the limiting magnitude of the plate in the band of the U B V RI system closest to the emulsionlter

combination estimated against a deep U B V RI sequence see text

plate date emulsion lter exp t lim mag

m

aO

m

aO

m

aO

m

aO

m

aO

m

aO

m

aO

m

aO

m

aO GG

m

aO GG

m

aO

m

aO GG

m

aO

m

aO GG

m

aO

m

PanRoyal GG

m

aO GG

m

aO GG

m

aO GG

m

PanRoyal GG

m

PanRoyal GG

m

aO GG

m

aO GG

m

PanRoyal GG

m

aO GG

m

TriX GG

m

aO GG

m

TriX GG

m

aO GG

m

aO GG

m

TriX GG

m

TriX GG

m

A aO GG

m

aD OG

m

aE RG

m

TriX GG

m

aO GG

m

aO GG

m

aO GG

m

TriX

IBVS

Our understanding of the physics of the eruptions of classical novae would undoubtedly

b enet from a broader knowledge of the photometric b ehaviour of their progenitor in

quiescence For example the detection frequency and brightness of DN outbursts may b e

used to estimate the masstransfer rate onto the accreting white dwarf prior to the nova

eruption cf Cannizzo

The Schmidt telescop es in use around the world generally have suciently faint limiting

magnitudes to b e of interest in the study of nova progenitors as we have shown for Nova

Cas and Nova Aql and such investigations on the largest p ossible set of novae

should b e encouraged

References

Cannizzo JK ApJ

Munari U Tomov T Hric L Hazucha P IBVS No

Tomov T Moro D Munari U IAU Circ No

Warner B Cataclysmic Variable Stars Cambridge Univ Press

Williams RE AJ

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CCD OBSERVATION OF THE FADING OF LQ Peg

T KATO M UEMURA

Dept of Astronomy Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp uemurakusastrokyotouacjp

LQ Peg PG was discovered as a UVexcess ob ject which was subse

quently conrmed as a cataclysmic variable Green et al Ferguson et al

A sp ectroscopic p erio d of hr was suggested by Ringwald Little had

b een known ab out its light variability until the discovery of a dramatic fading recorded on

photographs taken in Sokolov et al Although the ob ject can b e a p otential

candidate for the shortest p erio d VY Scltype star the lack of the corresp onding GCVS

type has partly made LQ Peg overlooked even after receiving the variable star designation

Kazarovets and Samus

The second historical fading of LQ Peg was detected by Watanabe The ob ject

was seen fainter than on July UT Up on this alert we started CCD

photometry to follow the fading episo de

The observations were done using an unltered ST camera attached to the Meade

cm SchmidtCassegrain telescop e The exp osure time was s The images were dark

TM

subtracted atelded and analyzed using the Java based PSF photometry package

developed by one of the authors TK The relative magnitudes of the variable were mea

sured against GSC R magnitude Henden and Honeycutt whose

C

constancy was conrmed by comparison with GSC USNO r magnitude

The resultant light curve is shown in Figure Each p oint represents a nightly av

eraged magnitude with an error bar indicating the standard error There was a slow

brightening trend after the apparent minimum on August JD The faintest

observed magnitude corresp onds to which is slightly brighter than the mini

mum Sokolov et al Then the brightness of the ob ject rose linearly with a rate

of mag d until September JD The rising b ecame slower thereafter

The general pattern and timescale of the recovery from minimum closely resemble those

observed in Sokolov et al and are consistent with the general characteristics

of VY Scltype novalike variables The ob ject has b een sparsely monitored by the VSOLJ

Variable Star Observers Leagues in Japan since without other noticeable fadings

Together with photographic and photo electric observations by Sokolov et al this

ob ject seems to sp end most of the time in bright states with relatively short excursions

to faint states

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture

IBVS

2

2.5 Rel. mag.

3

3.5

0 10 20 30 40 50 60

JD - 2451400

Figure Light curve of LQ Peg

References

Ferguson D H Green R F Lieb ert J ApJ

Green R F Ferguson D H Lieb ert J Schmidt M PASP

Green R F Schmidt M Lieb ert J ApJ Suppl

Henden A A Honeycutt R K PASP

Kazarovets E V Samus N N IBVS No

Ringwald F A PhD thesis Dartmouth College

Sokolov D A Shugarov S Yu Pavlenko E P in Cataclysmic Variables and

Related Ob jects eds A Evans and J H Woo d Kluwer Academic Publishers p

Watanabe T VSOLJ Variable Star Bul letin

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

CCD OBSERVATION OF THE SEPTEMBER OUTBURST

OF TY Vul

T KATO M UEMURA

Dept of Astronomy Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp uemurakusastrokyotouacjp

TY Vul is a rather obscure dwarf nova Downes et al presented an identication

based on the chart by Meinunger This identication suggests a very faint quiescent

counterpart Bond rep orted the sp ectral type of F which apparently refers to

the close companion describ ed b elow

Schmeer ab rep orted the apparently rstever outburst since the study by Mein

unger The rep orted maximum magnitude was V on September We

started timeresolved CCD photometry up on this alert The observations were done using

an unltered ST camera attached to the Meade cm SchmidtCassegrain telescop e

The exp osure time was s The images were darksubtracted atelded and ana

TM

lyzed using the Java based PSF photometry package developed by one of the authors

TK The relative uxes of the variable were measured against GSC USNO

r magnitude whose constancy was conrmed by comparison with GSC

USNO r magnitude The astrometry of the outbursting ob ject based on GSC

h m s  0 00

gave J which agrees with the cataloged p osition of

h m s  0 00

USNO J However Schmeer private

communication p ointed out that TY Vul and USNO make a close pair on

his CCD image The astrometric coincidence in our measurement may have partly b een

caused by the distortion of the GSC astrometric grid of this region

TY Vul and the companion b eing unresolved on our CCD images our measurements

give the combined light of the two stars Table and Figure show the nightly averaged

uxes

TY Vul rapidly faded on the night of September JD and the com

bined ux was virtually constant after September JD We determined the

averaged ux as representing the ux of the companion b etween the September and

observations and subtracted it from the outburst observations The rate of decline

determined from the rst two nights observations was mag d

Figure shows the enlarged light curve combined light on September A gen

eral decline consistent with the ab ove rate was observed during the run but no apparent

light mo dulation was detected

IBVS

.07

.06

.05

.04 Rel. mag. .03

.02

.01

0 24 26 28 30 32 34

HJD - 2451400

Figure Light curve of TY Vul

.08

.07

.06 Rel. mag.

.05

.04

.1 .12 .14 .16 .18 .2 .22 .24 .26 .28 .3 .32

HJD - 2451424

Figure Light curve of TY Vul on September

IBVS

Table Nightly averaged uxes of TY Vul

a a b c d

JD start JD end mean ux error N

a

JD

b

Combined ux TY Vul and companion

relative to GSC

c

Standard error of nightly average

d

Number of frames

The relatively large rate of decline the lack of light mo dulation and the large outburst

amplitude suggest the present outburst may b e a normal outburst of an SU UMatype

dwarf nova

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture

References

Bond H E PASP

Downes R Webbink R F Shara M M PASP

Meinunger I Vero Sternwarte Sonneberg

Schmeer P a vsnetalert circulation No

httpwwwkusastrokyotouacjpvsnetMailvsnetalertmsghtml

Schmeer P b vsnetalert circulation No httpwwwkusastrokyotouacjpvsnetMailvsnetalertmsghtml

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

PRECISE COORDINATES OF VARIABLE STARS

T KATO

Dept of Astronomy Faculty of Science Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp

This rep ort contains accurate J p ositions for variable stars discovered by

Homeister The variables stars were identied against computer plots of GSC

and USNO A catalogs The color information and IRAS PSC identication were also

examined in identifying red variables The source of identication in column Cat G

GSC GM average of GSC multiple entries U USNO A The table has

b een sorted in the increasing order of J right ascensions

V Ori S A susp ected UG star The co ordinates given in Downes et al

do not agree well with the Homeisters chart The identication given here may

b e more likely apart from the lack of corresp onding description by Homeister and the

relatively red color

LN Aur S Two p ositions are given The rst p osition refers to a red star near

the p osition whose magnitude agrees with Homeisters description on the blue POSS



plate However the second identication LN Aur agrees b etter with Homeisters

nding chart but has a rather blue color More examination is needed

Detailed information of identications other catalog identications are available from

the VSNET archive vsnet

httpwwwkusastrokyotouacjpvsnetMailvsnetmsghtml etc

The author is grateful to the USNO PMM team for making USNO A CDROMs

available to the author This work is partly supp orted by the GrantinAid for Scientic

Research of the Japanese Ministry of Education Science Culture and Sp orts

References

Downes R Webbink R F Shara M M PASP

Homeister C Astron Nach

IBVS

Table Precise co ordinates of variable stars

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

FH And : : G V Per : : U

V Cas G IQ Tau G

NS And GM IR Tau U

V Cas G IW Tau GM

V Cas U V Ori G

FI And G V Ori GM

VV Psc U V Aur G

V Cas GM V Ori U

V Cas GM V Aur G

VW Psc GM LM Aur G

V Cas U V Ori U

V Cas G V Aur G

OZ Per G V Ori G

V Cas G V Ori U

RY Tri GM V Ori G

RZ Tri GM V Ori U

SS Tri G PY Aur U



PQ Per U LN Aur U

V Per U LN Aur U

ST Tri GM V Aur U

PT Per U PZ Aur U

V Cas GM V Aur GM

V Per G LO Aur U

QR Per G LQ Aur U

V Per G LS Aur U

QZ Per U V Aur G

V Per G V Aur G

V Per U LT Aur G

V Per U LU Aur G

IL Tau G QS Aur G

V Per GM MX Aur G

V Per U QT Aur G

V Tau GM V Aur U

V Per U V Aur G

IBVS

Table cont

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

V Aur : : G V Cyg : : G

LX Aur U V Cyg GM

V Mon U V Cyg U

HR Hya G V Cyg U

HT Hya G V Cyg G

IU Hya G V Cyg G

V Her G V Cyg G

V Her GM V Cyg GM

V Oph G V Cyg G

V Oph U V Cyg G

V Oph U GR Sge U

V Oph U GZ Del U

V Oph U HH Del G

V Oph U HV Del U

V Her U HX Del GM

V Her G HZ Del G

V Lyr G I I Del U

V Lyr U IK Del U

V Lyr U HT Del U

V Lyr U LN Del G

V Lyr U V Cyg GM

CC Dra G GO Lac U

V Lyr U GQ Lac U

V Lyr G HN Cep U

EG Dra G GS Lac U

EH Dra G HO Cep U

V Lyr U GW Lac U

V Lyr U GY Lac U

V Cyg U V Cas U

CH Dra U V Cas U

V Cyg G V Cas U

V Cyg GM V Cas U

V Cyg G

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

PRECISE COORDINATES OF VARIABLE STARS

T KATO

Dept of Astronomy Faculty of Science Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp

This rep ort contains accurate J p ositions for variable stars discovered by

Homeister The variables stars were identied against computer plots of GSC

and USNO A catalogs The color information and IRAS PSC identication were also

examined in identifying red variables The source of identication in column Cat G

GSC GM average of GSC multiple entries U USNO A UM average of

USNO A multiple entries The table has b een sorted in the increasing order of J

right ascensions

V Oph S V Cyg S doubtful identication one of p ossible

candidates

HQ Sge S double star The southeastern bluer comp onent is selected

KO Vul S doubtful identication one of candidates Homeisters description

is slightly ambiguous

V Cyg S the identity of S with V Cyg is slightly unclear

Detailed information of identications other catalog identications are available from

the VSNET archive vsnet

httpwwwkusastrokyotouacjpvsnetMailvsnetmsghtml etc

The author is grateful to the USNO PMM team for making USNO A CDROMs

available to the author This work is partly supp orted by the GrantinAid for Scientic

Research of the Japanese Ministry of Education Science Culture and Sp orts

Reference

Homeister C Astron Nach

IBVS

Table Precise co ordinates of variable stars

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

NSV : : U CI Com : : GM

NSV U DE Vir G

V Cas G NSV G

V Cas U DH Vir G

V Cas G DG Vir U

V Cas U GN Vir G

NSV GM DI Vir U

V Cas U NSV GM

NSV GM V Her U

NSV GM NSV G

NSV GM V Her GM

V Cas U V Her U

V Cas U V Her GM

NSV G V Oph U

NSV G NSV G

V Cas G NSV U

NZ Cas G NSV G

NSV G NSV G

PU Per U V Her U

PV Per U V Her U

V Per G V Oph G

V Per G V Her GM

PZ Per U V Her G

V Per G NSV G

NSV G V Her U

IP Tau GM V Her G

V Ori G NSV G

V Aur U V Oph U

LL Aur U V Oph G

V Aur U V Her G

V Ori GM NSV G

PX Aur U V Her G

V Ori U V Oph U

V Ori U NSV G

V Ori U V Her U

V Ori U NSV G

LP Aur G V Oph U

V Aur U V Oph U

NSV G V Oph U

OO Gem G NSV GM

V Aur G NSV G

LV Aur G V Her U

V Ori U V Oph U

V Ori U V Oph U

V Aur U NSV G

LW Aur GM V Oph U

OP Gem G NSV G

KK Gem G NSV G

OQ Gem U EP Ser U

KO Gem U V Oph U

OR Gem G V Oph U

KT Gem U NSV G

NSV G NSV G

NSV G V Oph U

NSV GM V Oph GM

IBVS

Table cont

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

NSV : : G V Aql : : G

V Oph U V Aql G

V Oph G V Aql U

V Her U V Aql U

V Her U V Aql U

V Her U FU Sge U

V Oph U FV Sge G

NSV GM V Aql U

V Oph U V Aql U

NSV U NSV GM

AZ Ser G V Aql U

V Lyr G V Aql G

V Oph G NSV G

V Oph U NSV GM

V Oph U V Aql U

V Oph U NSV G

NSV GM NSV GM

V Lyr G FW Sge U

V Oph U HO Sge U

V Oph U KL Vul U

V Oph U V Aql U

V Lyr UM FX Sge U

V Her U KM Vul G

V Oph U HP Sge U

V Oph U V Aql G

EY Ser U HQ Sge U

V Oph U V Aql U

V Oph U FY Sge U

V Oph U V Cyg U

V Oph U FZ Sge U

V Oph U KO Vul U

V Oph U V Aql U

V Her U GG Sge U

V Oph U V Aql U

V Lyr G NSV GM

V Oph U V Aql U

V Oph U V Aql U

V Oph U V Aql G

V Oph U V Cyg GM

V Lyr U V Aql U

V Oph U V Cyg G

V Oph U GH Sge G

V Oph GM V Aql U

NSV U V Cyg G

V Her G GI Sge U

V Aql U V Aql G

V Aql U NSV GM

NSV GM NSV U

NSV G GK Sge U

V Aql G V Aql U

V Aql GM V Cyg G

V Aql G NSV G

V Aql U GM Sge U

V Aql GM V Aql U

V Aql U NSV U

IBVS

Table cont

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

NSV : : U V Cyg : : U

V Cyg G V Cyg G

NSV GM V Cyg U

NSV G V Cyg U

NSV G NSV GM

V Aql U V Cyg U

KQ Vul U NSV U

NSV G V Cyg U

NSV GM V Cyg U

NSV GM V Cyg U

NSV G NSV U

NSV G V Cyg U

NSV GM NSV U

GP Sge G V Cyg U

KS Vul U V Cyg U

GQ Sge GM V Cyg U

KT Vul U NSV U

V Aql G NSV G

V Aql GM NSV U

NSV GM NSV G

NSV U HH Lac U

V Aql U GZ Lac U

KU Vul U HI Lac U

KV Vul U V Lac U

KW Vul U V Cas U

KX Vul U NSV GM

V Aql G NSV G

V Cyg U V Cas U

NSV G V Cas U

NSV U V Cas U

HI Del U V Cas U

KY Vul U NSV U

KW Del G FY And U

HL Del U FZ And U

HK Del U V Cas U

KZ Vul U V Cas U

V Cyg U V Cas U

NSV G V Cas U

NSV G NSV G

HN Del U V Cas U

NSV GM V Cas G

NSV G V Cas GM

HO Del U NSV U

V Cyg U V Cas U

NSV GM V Cas G

HQ Del U NSV U

V Cyg G NSV G

KY Del GM NSV GM

V Cyg U NSV GM

KZ Del G NSV GM

LL Del G NSV GM

V Cyg GM V Cas U

HS Del U NSV G

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

PRECISE COORDINATES OF VARIABLE STARS

T KATO

Dept of Astronomy Faculty of Science Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp

This rep ort contains accurate J p ositions for variable stars discovered by

Homeister The variables stars were identied against computer plots of GSC

and USNO A catalogs The color information and IRAS PSC identication were also

examined in identifying red variables The source of identication in column Cat G

GSC GM average of GSC multiple entries U USNO A UM average of

USNO A multiple entries The table has b een sorted in the increasing order of J

right ascensions

V Mon S MT Pup S V Oph S GU Sge S

Homeisters chart is distorted Possible candidate is given

V Her and V Her S and S original charts were interchanged

Downes et als p osition for V Her is slightly dierent from that of the p ossible

USNO counterpart given in the table

Detailed information of identications other catalog identications are available from

the VSNET archive vsnet

httpwwwkusastrokyotouacjpvsnetMailvsnetmsghtml etc

The author is grateful to the USNO PMM team for making USNO A CDROMs

available to the author This work is partly supp orted by the GrantinAid for Scientic

Research of the Japanese Ministry of Education Science Culture and Sp orts

References

Downes R Webbink R F Shara M M PASP

Homeister C Astron Nach

IBVS

Table Precise co ordinates of variable stars

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

V Per : : U V Ori : : UM

V Per G MT Aur U

V Per G MU Aur U

NSV G MV Aur G

OV Tau U V Ori G

V Per G V Ori G

NSV G LO Gem G

V Per G LP Gem G

NSV G V Mon U

V Per U V Mon U

NSV G LV Gem G

V Ori U LW Gem U

NSV G NSV U

NSV GM FG CMa G

V Tau U NSV GM

V Ori U V Mon U

V Ori G V Mon U

V Tau U NSV G

V Ori U NSV U

V Ori U FI CMa U

V Ori G LX Gem G

V Tau U LY Gem U

NSV G LZ Gem U

NSV G NSV GM

MO Aur U MM Gem U

MP Aur U MN Gem U

V Tau U MO Gem G

V Ori U V Mon U

V Ori U V Mon G

V Ori U MQ Gem U

MR Aur U FK CMa U

NSV GM V Mon G

NSV U NSV G

V Tau U MS Gem U

NSV U V Mon GM

V Tau GM MT Gem U

IBVS

Table cont

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

MU Gem : : G NSV : : GM

FL CMa U NSV GM

MV Gem U V Mon G

NSV G MU Pup GM

V Mon U MT Pup U

NSV G MV Pup GM

MW Gem U NSV G

MX Gem U DQ Vir G

MZ Gem U DR Vir G

NN Gem G DS Vir G

FO CMa U V Her G

AV CMi GM V Her G

FP CMa G V Her U

V Mon U V Her G

AW CMi U V Her G

AX CMi GM V Her G

NSV GM NSV GM

AY CMi G V Her U

NSV U V Her GM

NSV G V Her G

NSV U V Her G

V Mon U V Her U

V Mon U NSV G

NSV G V Her U

MP Pup GM V Her U

NSV GM V Her U

NSV GM V Her G

V Mon G V Her U

NSV GM V Her U

NSV U NSV G

NSV U NSV G

MR Pup U V Her G

MS Pup U V Her G

NSV G V Her U

NSV U V Her G

V Mon U V Her G

IBVS

Table cont

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

V Her : : G V Her : : U

V Her G V Oph U

NSV GM V Oph U

NSV GM NSV G

V Her U V Oph U

V Her U V Oph U

V Her G NSV G

NSV G NSV G

V Her U NSV GM

V Her U NSV G

V Her G V Her G

NSV G V Oph U

V Oph U V Her GM

V Oph U V Oph U

V Oph G V Oph U

V Oph U NSV GM

V Her G NSV G

NSV G NSV U

NSV G V Oph GM

NSV G V Oph G

V Oph U V Oph GM

NSV G V Oph GM

NSV G FG Ser GM

V Her G NSV G

V Oph GM NSV GM

V Oph U NSV U

V Her U GS Sge U

NSV U GT Sge U

NSV G GU Sge U

NSV U NSV U

NSV G NSV U

NSV U NSV GM

NSV U GW Sge U

V Oph U NSV U

NSV G NSV GM

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

PRECISE COORDINATES OF VARIABLE STARS

T KATO

Dept of Astronomy Faculty of Science Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp

This rep ort contains accurate J p ositions for variable stars discovered by

Hoeit The variables stars were identied against computer plots of GSC and

USNO A catalogs The color information and IRAS PSC identication were also

examined in identifying red variables The source of identication in column Cat G

GSC GM average of GSC multiple entries U USNO A The table has

b een sorted in the increasing order of J right ascensions

The identications for the following stars are slightly uncertain b ecause of the high

density of stars andor chart distortions V Sgr V Sgr V Sgr V Sgr

V Sgr V Sgr V Sgr V Sgr V Sgr V Sgr V Sgr V

Sgr V Sgr V Sgr V Sgr V Sgr V Sgr V Sgr V Sgr

V Sgr V Sgr V Sgr V Sgr V Sgr V Sgr V Sgr V

Sgr V Sgr V Sgr

Detailed information of identications other catalog identications are available from

the VSNET archive vsnet

httpwwwkusastrokyotouacjpvsnetMailvsnetmsghtml etc

The author is grateful to the USNO PMM team for making USNO A CDROMs

available to the author This work is partly supp orted by the GrantinAid for Scientic

Research of the Japanese Ministry of Education Science Culture and Sp orts

Reference

Hoeit D IBVS No

IBVS

Table Precise co ordinates of variable stars

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

V Sgr : : GM V Sgr : : G

V Sgr G V Sgr U

V Sgr U V Sgr U

V Sgr G V Sgr G

V Sgr G V Sgr G

V Sgr GM V Sgr U

V Sgr U V Sgr U

V Sgr G V Sgr G

V Sgr G V Sgr GM

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr G V Sgr U

V Sgr GM V Sgr G

V Sgr G V Sgr U

V Sgr GM V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr GM

V Sgr G V Sgr G

V Sgr GM V Sgr G

V Sgr GM V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr G

V Sgr G V Sgr U

V Sgr G V Sgr G

V Sgr GM V Sgr U

V Sgr G V Sgr G

V Sgr U V Sgr G

V Sgr U V Sgr U

V Sgr G V Sgr U

V Sgr G V Sgr G

V Sgr U V Sgr G

V Sgr U V Sgr G

V Sgr G V Sgr U

IBVS

Table cont

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

V Sgr : : G V Sgr : : GM

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr G V Sgr GM

V Sgr U V Sgr G

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr G V Sgr U

IK Sgr U V Sgr U

V Sgr G V Sgr U

V Sgr U V Sgr U

IM Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr G

V Sgr G V Sgr GM

V Sgr U V Sgr GM

V Sgr GM V Sgr U

V Sgr G V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr G V Sgr G

V Sgr U V Sgr G

V Sgr G V Sgr G

V Sgr G V Sgr U

V Sgr U V Sgr G

V Sgr GM V Sgr G

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr GM V Sgr G

V Sgr U V Sgr U

V Sgr U V Sgr U

V Sgr U YY Sgr GM

V Sgr U V Sgr U

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

POSSIBLE IDENTIFICATION OF MisV AND NSV

1 2 3

SEI ICHI YOSHIDA KENICHI KADOTA TAICHI KATO

1

MISAO Pro ject Miyawada Fujishiromachi Kitasomagun Ibaraki Japan

email seiichimuraokainfowasedaacjp

2

MISAO Pro ject Koshikiya Ageo City Saitama Japan

email kenickastroartscojp

3

Dept of Astronomy Kyoto University Kyoto Japan email tkatokusastrokyotouacjp

This rep ort discusses the p ossible identication of MisV one of new variable stars

discovered in the course of the MISAO Pro ject and NSV one of the susp ected vari

able stars in the NSV catalog New Catalogue of Susp ected Variable Stars Supplement

Kazarovets et al

In the course of variable star survey based on the MISAO Pro ject observations the vari

h m s  0 00

able brightness of USNOA RA Decl

magR magB was discovered and named as MisV Yoshida

et al

NSV is arcsec from MisV At the p osition of NSV there is a star

h m s  0 00

USNOA RA Decl

magR magB see Figure

Table shows the photometry of these two stars obtained automatically by the PIXY

system from unltered CCD images taken by Kadota b etween May and September

The magnitudes were measured using the USNOA catalog based on a preliminary V

magnitude calculated from R and B magnitude in the catalog based on Katos

equation

V R B R

Further details are the same as describ ed in Yoshida and Kadota These obser

vations conrmed the variability of USNOA while USNOA

was constant within the error

In order to conrm the color of the two stars we measured relative colors of these stars

by comparing images with an Rlter and an IRblo cking lter Table Red stars

are relatively fainter through an IRblo cking lter The data in the USNOA catalog

of these two stars implies b oth stars are red Our observations conrm that USNOA

is evidently red while USNOA is not red

The nding chart of NSV is given in Margoni and Stagni The star

lab elled as NSV on the chart is identical with USNOA However

there is a remark on NSV that is very bright in the infrared This do es not agree

with the result of our observations

IBVS

Table Photometry unltered CCD

JD USNOA USNOA

Table Photometry ltered CCD

Filter USNOA USNOA

none

R

IRblo cking

As a conclusion the identication of NSV with USNOA is

p ossibly a mistake and USNOA MisV is the true NSV

Because the nding chart of Margoni and Stagni was based on a blue photo

graphic plate USNOA a red star was to o faint to b e visible on the

chart This may explain why Margoni and Stagni lab elled the wrong star as the

variable

Figure A USNOA MisV

B USNOA

References

Kato T

httpwwwkusastrokyotouacjpvsnetMailvsnetchatmsghtml

Kazarovets E V Samus N N Durlevich O V IBVS No

Margoni R Stagni R AsAp Suppl

Yoshida S Kadota K IBVS No

Yoshida S Kadota K Kato T IBVS No

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

NEW VARIABLE STARS DISCOVERED IN THE MISAO PROJECT

V MisVMisV

SEI ICHI YOSHIDA KENICHI KADOTA TAICHI KATO

1

MISAO Pro ject Miyawada Fujishiromachi Kitasomagun Ibaraki Japan

email seiichimuraokainfowasedaacjp

2

MISAO Pro ject Koshikiya Ageo City Saitama Japan

email kenickastroartscojp

3

Dept of Astronomy Kyoto University Kyoto Japan email tkatokusastrokyotouacjp

This rep ort describ es new variable stars MisVMisV discovered in the

course of the MISAO Pro ject

These ob jects are detected automatically by the PIXY system as candidates of variable

stars from unltered CCD images taken by Kadota b etween April and August then

conrmed by Yoshida and Kadota Further details are same as describ ed in Yoshida and

Kadota

Table contains the list of new variable stars The p osition and magnitude are mea

sured using USNOA catalog The magnitude is based on a preliminary V magnitude

calculated from R and B magnitude in the catalog based on Katos equation

V R B R

The nding charts are available electronically as fnnneps where nnn refers to the

serial number assigned to the star in the rst column of Table

NSV is arcmin from MisV However it was detected on our unltered

CCD image as around mag Therefore MisV is another new variable star

EM Oph is arcmin from MisV QY Oph is arcmin from MisV IN Sco

is arcmin from MisV No star brighter than mag was detected at these p osi

tions on our unltered CCD images However considering the large distance MisV

MisV and MisV are probably new variable ob jects

MisV is lo cated at a distance of arcsec from the cataloged p osition of the

obscure nova DZ Ser A slight uncertainly of the co ordinates rep orted among existing

references Duerb eck may have led to a p ossible identication More extensive

study of the new variable and the comparison with the discovery material of DZ Ser are

needed to clarify the situation

References

Duerb eck H W Space Sci Rev

IBVS

Kato T

httpwwwkusastrokyotouacjpvsnetMailvsnetchatmsghtml

Yoshida S Kadota K IBVS No

Yoshida S Kadota K Kato T IBVS No

Yoshida S Kadota K Kato T IBVS No

Yoshida S Kadota K Kato T IBVS No

Yoshida S in preparation

Table List of New Variable Stars

Unltered

CCD Mag

Co de RA J Decl Type Identied with

Max Min

h m s  0 00

MisV : : USNOA

IRAS

MisV USNOA

IRAS

MisV IRAS

MisV IRAS

MisV IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV

MisV USNOA

MisV USNOA

MisV USNOA

MisV

MisV

MisV SR USNOA

MisV USNOA

MisV SR USNOA

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV IRAS

MisV USNOA

IRAS

MisV GSC

USNOA IRAS

IBVS

Table cont

Unltered

CCD Mag

Co de RA J Decl Type Identied with

Max Min

h m s  0 00

MisV : : IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV SR USNOA

IRAS

MisV M GSC

USNOA

IRAS

MisV SR IRAS

MisV IRAS

MisV IRAS

MisV IRAS

MisV USNOA

IRAS

MisV IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV IRAS

MisV IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV IRAS

MisV USNOA

MisV IRAS

MisV IRAS

MisV SR USNOA

IRAS

MisV USNOA

IRAS

MisV USNOA

IRAS

MisV SR GSC

USNOA IRAS

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

CCD PHOTOMETRY OF THE FEBRUARY SUPEROUTBURST

OF CT Hya

1 2 3 1

T KATO S KIYOTA R NOVAK K MATSUMOTO

1

Dept of Astronomy Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp katsurakusastrokyotouacjp

2

Variable Star Observers League in Japan Azuma Tsukuba Japan

email skiyotaabrarcgojp

3

Nicholas Cop ernicus Observatory Kravhora Brno Czech Republic

email rudolfnphysicsmunicz

CT Hya was discovered as a dwarf nova by Homeister The SU UMatype

nature of this dwarf nova was rst revealed by Nogami et al who discovered

d

sup erhumps with a p erio d of although there remained some ambiguity in the

alias selection Nogami et al suggested that CT Hya is an intermediate ob ject

b etween ordinary SU UMa stars and WZ Sge stars Up on the alert of a bright outburst on

February R Stubbings VSNET we underto ok a timeresolved CCD photometry

campaign Table summarizes the observation runs

The observations at Kyoto were done using an unltered ST camera attached to the

Meade cm SchmidtCassegrain telescop e The exp osure time was s The images

TM

were darksubtracted atelded and analyzed using the Java based ap erture and

PSF photometry package developed by one of the authors TK The magnitude of the

variable was measured relative to GSC Tycho V B V

whose constancy was conrmed by comparison with GSC Tycho V

B V

Brno observations were p erformed on a cm Newtonian telescop e using an ST

camera and an I band KronCousins lter During the outburst when star was fading we

changed exp osure times which are given in Table Images were darksubtracted at

elded and analyzed using Munidos photometry package Novak The magnitude of

variable was determined relative to GSC which shows no variability up to mag

limit Due to cloudy weather some of the CCD frames were omitted from nal datasets

and in some cases the instrumental magnitude error was quite large These observations

were also omitted

Tsukuba observations were done using an AP CCD attached to a cm Schmidt

Cassegrain telescop e A Johnson V lter was adopted The comparison star GSC

was used to calibrate the magnitude The constancy of the comparison was conrmed by

using a check star GSC

All the observations were rst shifted by constant magnitudes to b est match the

Tsukuba V system The dierences in passbands will not seriously aect the p erio d

IBVS

Table Summary of observations

a a b c d

start JD end JD observatory band N t

Kyoto C

Kyoto C

Tsukuba V

Brno I

C

Kyoto C

Tsukuba V

Brno I

C

Kyoto C

Kyoto C

Brno I

C

Kyoto C

Tsukuba V

Brno I

C

Brno I

C

Kyoto C

Kyoto C

Kyoto C

Kyoto C

Kyoto C

a

JD

b

C for unltered CCD

c

Number of frames

d Exp osure time s

14

15

16

Rel. mag. 17

18

19

20 24 26 28 30 32 34 36 38 40 42 44

HJD - 2451200

Figure Overall light curve of CT Hya

IBVS

analysis of outbursting dwarf novae whose colors are known to b e close to B V

Figure illustrates the resultant overall light curve of the present observations Five con

secutive Kyoto observations were averaged to get one p oint corresp onding to an eective

exp osure time of s Before February JD individual observations are

plotted after the decline nightly averages with error bars are plotted instead The sup er

outburst plateau stage February was analyzed after subtracting the linear decline

trend using the Phase Disp ersion Minimization PDM metho d Stellingwerf

1.05

1

.95

theta .9

.85

.8 P = 0.0664

10 12 14 16 18 20

Frequency (cycle/day)

Figure Period analysis of CT Hya

The result of p erio d analysis is given in Figure The p erio d analysis was applied to

Kyoto and Tsukuba data since some ambiguity remained in Brno observations caused

by clouds or p otential unsolved problem as describ ed later The b estdetermined sup er

hump p erio d is  d which corresp onds to the longer oneday alias given by Nogami et al

-.15

-.1

-.05

Rel. mag. 0

.05

.1

-.4 -.2 0 .2 .4 .6 .8 1 1.2 1.4

Superhump phase

Figure Sup erhump prole of CT Hya

Figure shows the averaged sup erhump prole

IBVS

.02

.01

O - C 0

-.01

-.02 0 20 40 60 80 100

Cycle number

Figure Sup erhump O C diagram

Sup erhump maxima times were measured by eye and the leastsquares tting yielded

the quadratic p olynomial equation

MaxHJD E  E

where E is the cycle number see also Figure The change in the sup erhump p erio d was

negligible in contrast to usual SU UMa stars which show a rather common sup erhump

p erio d decrease at a rate of P P   This lack of p erio d decrease is another

common prop erty of shortp erio d SU UMa stars Kato et al We must note the

Brno observations on HJD were disregarded in this O C analysis b ecause this

observation showed a nearly reversed sup erhump phase The reason is left unsolved either

there was a large change in p erio d or phase or there may have b een an unknown problem

in time recording The problem should b e solved in the next sup eroutburst

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture and Sp orts TK Part of this

work is supp orted by a Research Fellowship of the Japan So ciety for the Promotion of

Science for Young Scientists KM

References

Homeister C Astron Nachr

Kato T Nogami D Baba H Matsumoto K in Wild Stars in the Old West

eds S Howell et al ASP Conf Series p

Nogami D Kato T Hirata R PASJ

NovakR httpaltamiraasucasczmunidos

Stellingwerf R F ApJ

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

IDENTIFICATION AND CCD PHOTOMETRY OF LUYTENS GM Sgr

T KATO M UEMURA

Dept of Astronomy Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp uemurakusastrokyotouacjp

There have b een confusion in the correct identication of Luytens variable HV

which was originally given the GCVS name GM Sgr Goranskij discovered an

eruptive variable star in its close vicinity which once to ok over the GCVS nomenclature

GM Sgr The variable the aring Xray transient was later given a new variable star

name V Sgr Samus

In this pap er we provide the identication chart and CCD photometry of Luytens

GM Sgr USNOA Hazen Morel based on our CCD

images used for photometry of V Sgr Kato et al The CCD observations were

done using an unltered ST camera attached to a cm SchmidtCassegrain telescop e

at Kyoto University The exp osure time was s The images were darksubtracted

TM

atelded and analyzed using the Java based ap erture photometry package developed

by one of the authors TK The magnitudes of GM Sgr were determined using the

GSC Tycho V B V whose constancy was conrmed by

comparison with GSC

Figure Identication chart of Luytens GM Sgr

IBVS

2.5

3

Rel. mag.

3.5

4

410 420 430 440 450 460 470 480 490

JD - 2451000

Figure Light curve of GM Sgr

Figure shows the comparison of CCD images taken on August left and

Octob er right North is approximately up The ob ject markedly brightened

b etween these two exp osures

Figure represents the light curve of GM Sgr The magnitudes are shown relative to

GSC A monotonous rise of mag during d is evident The ob ject seems

to have reached a maximum in late Octob er Using the estimated R magnitude

C

of the comparison the observed range of GM Sgr b ecomes R though the

C

actual minimum can b e fainter From the observed light variability we have conrmed

the Luytens original classication as a longp erio d variable

This work is partly supp orted by the GrantinAid for Scientic Research

of the Japanese Ministry of Education Science Culture and Sp orts TK

References

Goranskij V P Astron Tsirk No

Goranskij V P IBVS No

Hazen M vsnetchat circulation No

httpwwwkusastrokyotouacjpvsnetMailvsnetchatmsghtml

Kato T Uemura M Stubbings R Watanabe T Monard B IBVS No

Morel M vsnetchat circulation No

httpwwwkusastrokyotouacjpvsnetMailvsnetchatmsghtml

Samus N N IAUC No

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

REDUCED AMPLITUDE OF V OPHIUCHI

ERIC G HINTZ MAUREEN L HINTZ MICHAEL D JONER AND LISA A JONER

Brigham Young University Dept of Physics Astronomy Provo Utah USA

email do ctorshapleybyuedu romanatardisbyuedu mastertardisbyuedu

h m s  0 00

V Ophiuchi GSC was

rst rep orted as a variable star S Oph by Gotz The star was observed on

photographic plates over a span of d From the data Gotz classied the star as an

d m

RRc variable with a p erio d of an amplitude of and an average magnitude

of m Gotz found that V Oph had two distinct amplitudes for the

p

maxima of and mag From the description in Gotz the star may have

shown oscillations similar to those found in stars like SX Pho enicis or other multiperio dic

variable stars Since that time the star has received eectively no attention

Because of its high amplitude and p ossible similarity to SX Phe we chose to observe

V Oph in August These observations were made with the Burrell Schmidt Tele

scop e hereafter BST at Kitt Peak National Observatory with the SKA CCD camera

through a V lter mo deled after Bessell Four nights of supplemental data were ob

00

tained with the David Derrick Telescope of the Orson Pratt Observatory at Brigham

Young University hereafter DDT These data were secured with a Pictor XT CCD

mounted at the Newtonian fo cus of the DDT through the same V lter mentioned ab ove

The four nights ranged from May until July The CCD eld for the DDT is

shown in Fig

All frames were reduced using standard IRAF functions Dierential magnitudes were

determined using the eight comparison stars and the metho ds detailed in Hintz et al

A mean apparent magnitude of hm i was determined for V Oph from

V

one night of data on which observations of SA Landolt were also secured

This is dierent from the published photographic magnitude of m even with a

p

reasonable color correction We were condent in our identication of V Oph from the

nder in Gotz but carefully checked all surrounding stars of similar brightness to

determine if the star had b een misidentied However no other short p erio d variables

were found in the region We concluded that we indeed monitored the correct star

Using the Period package the rst term of a Fourier series was t to all ve nights

d d

of data From this we determined a p erio d of and an amplitude of

This is clearly dierent than the p erio d rep orted by Gotz From

the times of maximum light list in Gotz we used a linear regression to recalculate

d d

the p erio d A p erio d of was found

IBVS

0 0

Figure CCD eld of V Oph with comparison stars lab eled The eld of view is 

Figure Phased light curve of V Ophiuchi The solid line is the rst term of a Fourier t

IBVS

Table New Times of Maximum Light for V Ophiuchi

HJD

Telescope Detector Cycle

BST SKA

DDT Pictor

DDT Pictor

DDT Pictor

DDT Pictor

DDT Pictor

This p erio d is dierent than b oth the Gotz value and that given by our Fourier

t Using the p erio d from the Fourier t all ve nights of new data were phased as shown

in Figure Matching each nights data to the phased curve six times of maximum light

were determined These times are collected in Table From these six times of maximum

light a new ephemeris for V Oph was determined as given in Eq

HJD E

max

This agrees with the value from the Fourier t but is clearly dierent than the value

from the Gotz data The exact nature of the p erio d change in V Oph is unclear due

to the lack of available data However there has b een a change at some p oint during the

last years

In addition to the p erio d change there was a substantial decrease in the amplitude

of V Oph A less dramatic example of a similar eect was seen in V Orionis by

Hintz et al For comparison with V Ori two pieces of information would b e

useful Stromgrenindices and the rotational velocity The Stromgrenindices would give

V Ophs p osition with resp ect to the instability strip The rotational velocity of V

Oph should b e compared to the values for other high amplitude Scuti stars Solano

Fernley found a rotation velocity for V Ori of km s This is the highest

measured rotation rate for any high amplitude Scuti star The dierence in rotation

velocities b etween high and low amplitude Scuti stars has b een discussed by Breger

Andreasen and McNamara Perhaps the disparity in the relative

number of high and low amplitude Scuti stars can b e traced to the rotational velocity

Perhaps more stars started as high amplitude stars but have b ecome low amplitude stars

We thank the Brigham Young University Department of Physics and Astronomy for

their supp ort of research eorts using the BST We also wish to thank Case Western

Reserve University for the use of the BST We also acknowledge the assistance of Janet

Mattei and Ennio Poretti

References

Andreasen G K AA

Bessell M S PASP

Breger M ApJ

GotzW Vero Sternw Sonneberg

IBVS

Hintz E G Joner M D McNamara D H Nelson K A Mo o dy J W Kim C

PASP

Hintz E G Joner M D Kim C PASP

Landolt A U AJ

McNamara D H PASP

Solano E Fernley J AAS

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

DISCOVERY OF THE VARIABILITY OF GSC

GSC AND GSC

1 2;5 3;5 4;5

C LLOYD K BERNHARD P FRANK W MOSCHNER

1

Space Science Department Rutherford Appleton Lab oratory Chilton Didcot Oxon OX QX UK

email clastrobnscrlacuk

2

Kafkaweg A Linz Austria email klausb ernhardvp nat

3

D Velden Germany email frankveldentonlinede

4

D Lennestadt Germany email wolfgangmoschnertonlinede

5

Bundesdeutsche Arb eitsgemeinschaft f urVeranderliche Sterne eV BAV Munsterdamm D

Berlin Germany

Introduction

The new variable stars rep orted here have b een found as part of a programme to discover

and classify new variables using CCD observations of selected elds on the edge of the

northern Milky Way eg Bernhard et al Bernhard In this pap er the obser

vations of three new variables resulting from this programme are rep orted GSC

is an EA binary with a p erio d of days GSC and GSC are b oth

atype RR Lyrae variables with p erio ds of and days resp ectively These

stars have previously b een referred to as BeV BeV and BeV The observations

were made using a cm SchmidtCassegrain telescop e and an unltered Starlight Xpress

SX CCD camera The CCD camera uses a Sony ICXB chip which has a very broad

resp onse p eaking near A giving approximate Vband magnitudes dep ending on the

colour of the star Further details are given by Lloyd Bernhard Additional un

ltered observations of GSC have also b een obtained with an SBIG ST camera

on a cm RitcheyChretientelescop e WM

GSC

h m s  0 00

GSC J mag has b een observed nearly

times mostly during the March The magnitudes are given relative to GSC

mag and the second comparison star used was GSC mag The

magnitude dierence b etween the two comparisons stars  is remarkably

consistent with the GSC magnitudes The three sets of observations from the three

instruments describ ed ab ove have b een brought on to this magnitude scale by applying

small shifts to the two less extensive sets For the out of eclipse observations the shift is

well determined but for the other set which lies wholly within the secondary eclipse it

IBVS

Figure The observed light curve of GSC relative to GSC mag with the

three sets of observations indicated thus lled circles KB op en circles PF and op en squares WM

The light curve solution assuming two similar Atype stars with T T K R a

1 2 1

R a and i deg

2

is less certain To some extent the shift dep ends on the p erio d chosen but this has no

material eect on the light curve

From a p erio d analysis of the observations and the times of minimum only one clear

p erio d emerges days However for this type of light curve such a p erio d is physi

cally unrealistic so the true p erio d is taken to b e twice this value The observations show

GSC to b e an eclipsing binary with primary and secondary eclipses of 

and mag resp ectively although it is clear that the secondary minimum has not b een

completely covered see Figure There is no sp ectroscopic information and the USNO

A magnitudes of b and r do not provide any real constraint on the

system The ephemeris of primary minimum is

JDI    E

An attempt has b een made to mo del the system using the Light co de of Hill et al

A number of solutions have b een made using a wide range of temp eratures and

a range of mass ratios around unity The derived parameters are very insensitive to b oth

temp erature and mass ratio and not surprisingly suggest two stars of equal temp erature

and equal size So with T K xed and q xed T  K

R a  R a  and i  deg These values are representative

of a range of temp eratures Given the uncertainty in the temp eratures of the stars and

the lack of observations around one of the minima it is p ossible that further observations

will redene which is the primary eclipse From the relative radii it is p ossible to derive

an internally consistent set of the parameters P M and R for a pair of late Atype

mainsequence stars giving M  M R  R and T  K The solution with

the stars it this temp erature is shown in Figure

IBVS

Figure The light curve of GSC folded with a p erio d of days with a highorder

harmonic t sup erimp osed The magnitudes are given relative to GSC mag

GSC

h m s  0 00

GSC J mag has b een observed times

mostly in June and July Initially the observation were quite sparse but when

the shortp erio d nature of the variation b ecame clear several runs of approximately

observations were made The magnitudes are given relative to GSC mag

which proved constant relative to the second comparison star GSC mag

The p erio d analysis suers from some aliasing problems but ultimately only one p ossible

p erio d emerges The light curve plotted in Figure is clearly that of an atype RR

Lyrae and the ephemeris of maximum light is

JDmax    E

The coordinates of this star place it well ab ove the galactic plane at l and b

Adopting a mean magnitude V and M and assuming A mag kp c

V V

yields a distance of kp c and a height ab ove the galactic plane of kp c Combined

with the p erio d this distance places this star rmly in the eld halo p opulation

GSC

h m s  0 00

GSC J mag USNO A r b

has b een observed times mostly in August After the initial observations the

vast ma jority were taken in eight long runs The magnitudes are given relative to GSC

and GSC was used as the second comparison star The

observed magnitude dierence of mag is consistent with the GSC magnitudes The

p erio dogram shows one clear p erio d at days with relatively strong oneday aliases

although there is no real confusion The light curve is unmistakably that of an atype RR

Lyrae variable with an amplitude of  mag The light curve is plotted in Figure

IBVS

Figure The light curve of GSC folded with a p erio d of days with a highorder

harmonic t sup erimp osed The magnitudes are given relative to GSC mag

The ephemeris of maximum light is

JDmax    E

The galactic coordinates l and b and mean magnitude GSC  of

GSC are similar to the other RR Lyrae star rep orted here GSC and

the same analysis also p oints to GSC b elonging to the eld halo p opulation

References

Bernhard K Quester W Bastian U IBVS No

Bernhard K Der Sternenbote Astronomisches Buero A Wien p

Hill G Fisher WA Holmgren D AA

Lloyd C Bernhard K IBVS No

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

THE VARIABLE PERIOD OF V CASSIOPEIAE

BAV MITTEILUNGEN NR

1 1 1;2

FRANZ AGERER THOMAS BERTHOLD PETER KROLL

1

Bundesdeutsche Arb eitsgemeinschaft f urVeranderliche Sterne eV BAV Munsterdamm D

Berlin Germany Email agererzweiktonlinede b ertholdmtltonlinede

2

Sternwarte Sonneb erg Sternwartestr D Sonneb erg Germany Email pkstwtuilmenaude

V Cas sp ectr G GSC CSV S was discovered by

m

Homeister He announced it as a short p erio dic variable star b etween and

m

pg Further investigations on sky patrol plates were done by Perova

She found the star to b e of W UMa type and gave rst elements including a p erio d of

d

These elements could b e conrmed in an early pap er by Berthold

Using the minima given by Perova and new ones using sky patrol plates of Hartha

Observatory the following rened ephemeris has b een derived

d

Min I HJD E

With these elements V Cas is listed in the fourth edition of the GCVS Kholop ov et

al

FA recently made CCD photometry with a SBIG ST camera without lters attached

to a cm SCtelescop e from which minima times using the Kweevan Woerden

algorithm Kwee van Woerden could b e derived We also obtained a CCDbased

lightcurve given in Fig Since the amplitudes in Min I and Min II dier less than

the scattering from night to night we were not able to unambiguously distinct b etween

the resp ective minima We therefore left the denition of the primary minimum Min I

unchanged

In order to check the longterm b ehaviour of the p erio d and to bridge the gap b etween

the Hartha plates and the CCD measurements additional observations on sky patrol

plates of Sonneb erg Observatory were p erformed by TB They cover a p erio d of time

b etween JD and In order to obtain more accurate minimum times we

calculated mean lightcurves of consecutive subsections using ephemeris and thus

derived times of normal minima

As comparison stars the ones given in the pap er of Perova were used However we

derived new photographic magnitudes based on the HarvardGroningen SA

Perova GSC mpg Perova GSC mpg

a b

c d

IBVS

Figure O C diagram of all available minima according to ephemeris Symbols are identied as

follows 2 Photographic minima  Photographic normal minima of Berthold this pap er and 

CCD minima

Figure CCD light curve of V Cas according to elements

IBVS

Table Times of minima for V Cas ep o chs and residuals computed according to the ephemeris

and resp ectively

JD hel JD hel

 

W T Ep o ch O C Ref W T Ep o ch O C Ref

2 2 3 3

P F

P P

P P

F P

P F

P F

P F

E P

P E

P E

E P

P E

P E

E P

E P

P E

E P

P E

P E

E P

P E

P E

P

P

P

P

P

P

P

P

P



P denotes photographic minima F photographic normal minima and E CCD observed minima

Those marked with got reduced weight

Perova Berthold Berthold this pap er Agerer this pap er

Diethelm

As it is clearly to b e seen the p erio d of V Cas is signicantly changing For

describing such a b ehaviour two dierent approaches can b e made we assume the

p erio d was constant during certain p erio ds of time with distinct p erio d jumps in b etween

we apply a continuously increasing changing p erio d with a quadratic O C t

Assuming two consecutive constant p erio ds the following set of linear elements can b e

derived

From JD approx to JD approx

d

Min I HJD E

From JD approx to JD last observed minimum

d

Min I HJD E

If Perovas rst moment of minimum is correct it is obvious that a further change has

o ccurred sometimes in the rst third of this century

Alternatively and the O C diagram suggests this strongly a weighted quadratic

IBVS

least squares t is also p ossible to achieve that yields the following elements

d

Min I HJD E

Based on the quadratic elements we can derive the rate of change of the p erio d as

d

dP p er orbital revolution Under the assumption that this change is caused

by mass exchange b etween the stars the mass transfer pro ceeds from the less massive

comp onent to the more massive comp onent since the p erio d increases If we knew the

stellar masses we were able to derive the mass transfer rate j mj using the wellknown

relation Kopal

 

dP j m j m

P m m

where m more massive comp onent and m represent the stellar masses Although

the CCD lightcurve Fig clearly indicates a close binary system and that one or

b oth stars must b e heavily distorted an estimate of the mass ratio is hard to achieve

Provided the stars are similar and thus assuming a mass ratio in the order of and

roughly a solar mass for b oth comp onents sp ectrum G we obtain a mass transfer

rate of M yr

The improved electronic version of the GCVS Kholop ov et al lists only other

ob jects of similar p erio ds days and sp ectra b etween F and G showing

WUMalike lightcurves VY Cnc UZ CMi RS Col and ER Vul Although describ ed

as EWDW this classication is erroneous in at least one case RS Col Insuciently

studied until to day UZ CMi might b e also a contact binary Giuricin Mardirossian

and Mezzetti ER Vul on the contrary is a shortp erio d RS CVntype star This

makes V Cas an interesting case to which more attention should b e paid We therefore

suggest timeresolved sp ectroscopy and multicolor CCD photometry of this ob ject

References

Berthold T Hartha Mitt

Diethelm R BBSAG Bul l No

Giuricin G Mardirossian F Mezzetti M Astron Astrophys Suppl Ser

Homeister C Erg Astron Nachr

Kholop ov PN et al httpwwwsaimsusudatabasehtml

Kopal Z Dynamics of close binary systems Reidel Dordrecht

Perova NB Perem Zvezdy

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

PRECISE COORDINATES OF VARIABLE STARS

T KATO

Dept of Astronomy Faculty of Science Kyoto University Kyoto Japan

email tkatokusastrokyotouacjp

This rep ort contains accurate J p ositions for variable stars discovered by

Homeister as a supplement to Kato The variables stars were identied

against computer plots of GSC and USNO A catalogs The color information and IRAS

PSC identication were also examined in identifying red variables The table has b een

sorted in the increasing order of J right ascensions The source of identication in

column Cat G GSC GM average of GSC multiple entries U USNO

A

NSV NSV NSV NSV NSV NSV NSV

NSV NSV NSV NSV V Aql identications are somewhat

ambiguous due to the chart distortion or crowding The most likely candidate has b een

selected

NSV and NSV S and S charts are interchanged

NSV and NSV identity with NSV and NSV resp ectively

should b e checked

Two identications of NSV stars with GCVS variables are found NSV GG

Mus and NSV V Lac

Detailed information of identications other catalog identications are available from

the VSNET archive vsnetid

httpwwwkusastrokyotouacjpvsnetMailvsnetidmsghtml etc

The author is grateful to the USNO PMM team for making USNO A CDROMs

available to the author This work is partly supp orted by the GrantinAid for Scientic

Research of the Japanese Ministry of Education Science Culture and Sp orts

References

Homeister C Astron Nach

Kato T IBVS No

IBVS

Table Precise co ordinates of variable stars

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

MW Per : : G NSV : : U

NSV U NSV U

NSV G NSV U

NSV G NSV G

NSV GM NSV U

NSV GM NSV U

NSV GM NSV U

NSV G NSV G

NSV U NSV G

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV G

NSV G NSV U

NSV U NSV U

NSV U NSV U

NSV G NSV U

NSV GM NSV U

NSV U NSV GM

NSV GM NSV U

NSV GM NSV U

NSV U NSV U

NSV G NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV UM

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV GM

NSV U NSV G

NSV G NSV G

NSV U NSV U

NSV G NSV G

NSV U NSV UM

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV GM NSV U

IBVS

Table cont

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

NSV : : G NSV : : U

V Her U NSV U

NSV GM NSV U

NSV U NSV U

NSV G NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV UM

NSV U NSV G

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV G NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV G NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV GM NSV U

NSV U NSV U

NSV G NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV GM

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV G NSV U

IBVS

Table cont

Desig RA Decl Cat Desig RA Decl Cat

h m s  0 00 h m s  0 00

NSV : : U NSV : : U

NSV G NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV G

NSV G NSV U

NSV U NSV U

NSV U NSV U

NSV G V Aql U

NSV U NSV U

NSV U NSV U

NSV U LP Vul U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NGC V U V Cyg U

NGC V U NSV U

NGC V U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV UM

NSV U NSV UM

NSV GM NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U V Cyg G

NSV U NSV G

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV U NSV U

NSV G NSV G

NSV U NSV U

NSV U NSV U

NSV U V Lac U

S U NSV U

NSV U NSV U

NSV U NSV G

COMMISSIONS AND OF THE IAU

INFORMATION BULLETIN ON VARIABLE STARS

Number

Konkoly Observatory

Budap est

November

HU ISSN

PHOTOMETRY OF THE ECLIPSING BINARY STAR

GSC RXS J

1

RM ROBB J WAGG A BERNDSEN AND L DESROCHES

1

Guest User Canadian Astronomy Data Centre which is op erated by the Herzb erg Institute of Astrophysics

National Research Council of Canada

Climenhaga Observatory Dept of Physics and Astronomy University of Victoria Victoria BC Canada

VW P email robbuvicca

Jenkner et al was found to have Ca HK emission in The star GSC

a survey by Beers et al Also called RXS J it was found to have

signicant XRay emission in a survey by the ROSAT satellite Bade et al In a

survey of high prop er motion stars it was classied as a K star by Stephenson

Rob ertson and Hamilton measured V B V and V I

Figure Finder chart lab eled with the GSC numbers

Plotted in Figure is the eld of stars observed with the automated m telescop e

and reduced in a fashion identical to that describ ed in Robb et al Tabulated

in Table are the stars identication numbers co ordinates J and magnitudes

from the Hubble Space Telescope Guide Star Catalog GSC Jenkner et al Our

dierential R magnitudes are calculated in the sense of the star minus GSC

For each star the mean of the nightly means is shown as R in Table The standard

deviation of the nightly means is a measure of the night to night variations and is called

IBVS

Table Stars observed in the eld of GSC

RA Dec GSC R Std Dev Std Dev

GSC No

J J Mag Mag Between Within

h m s  0 00

h m s  0 00

h m s  0 00

h m s  0 00

h m s  0 00

h m s  0 00

Std Dev Between in Table Brightness variations during a night were measured by

the standard deviation of the dierential magnitudes during a night The b est night is

had obvious variations tabulated in Table as Std Dev Within The star GSC

during a night and is thus a new eclipsing binary star

since There is no ambiguity in the determination of the orbital p erio d of GSC

d

three of the nights included more than one cycle Using data p oints within of the

minimum and the metho d of Kwee and van Woerden the helio centric Julian Dates

of minimum were found and are tabulated in Table On some nights observations were

made in more than one color and the separate times of minima are indicated

Table Times of Minimum of GSC

JD JD JD JD JD

R R I I R

R I V B R

R V I R

A t to these times gives the ephemeris

d d

HJD of Minima  E

where the uncertainties in the nal digit are given in brackets and the mean square error

d

of the t is

The dierential GSC GS C R magnitudes phased at this p erio d

are plotted in Figure with dierent symbols for each of the nights The asymmetry in

the maxima is indicative of star sp ots distributed asymmetrically over the surface of the

stars

CCD frames of the eld were obtained with B V and I lters to ascertain the

C

has B and V temp erature and brightness of the variable star The star GSC

magnitudes measured by the Hipparcos satellite ESA to b e V 

T

and B V  Measurements of GSC relative to this star give

T

V  and B V  at maximum light This B V is in agreement

with the measurements of the Hipparcos satellite ESA and also with Rob ertson

to and Hamilton From this color we estimate the sp ectral class of GSC

b e approximately KV Cousins in agreement with Stephenson

The light curve leads us to exp ect this to b e a nearcontact system Using Binmaker Bradstreet an example mo del light curve was made assuming the temp erature

IBVS

Figure R band light curve of GSC for

Figure R band normal p oints with curve from an example mo del of the eclipsing system

IBVS



of the hot star to b e K the mass ratio of and the latitude of the sp ot of



The data are b est tted with an inclination of and relative radii of and



The temp erature of the co ol star was adjusted to K and a sp ot in radius at



a longitude of was added to get the t seen in Figure Considering the cycle to

cycle variations seen in the light curve this is a satisfactory t The uncertainty in the



inclination is ab out  and the dierence in temp erature and sp ot diameter are known

to ab out 

Figure Threedimensional mo del of the nearcontact system at phase

The relative sizes and shap es of the comp onents of the system and the sp ot are shown

in Figure again using Binmaker Bradstreet

is therefore a nearcontact eclipsing system with latetype com The star GSC

p onents and at least one sp ot Photometric observations should b e continued to monitor

light curve changes due to sp ot migration ares and p erio d changes Sp ectroscopic ob

servations have b een started to determine a precise sp ectral class for the system and to

measure radial velocities to determine the masses and the scale of the system

References

Beers T C Bestman W and Wilhelm R AJ

Bade N Engels D Voges W Beckmann V Boller Th Cordis L Dahlem M

Englhauser J Molthagen K Nass P Studt J Reimers D AA Sup

Bradstreet DH Binary Maker User Manual Contact Software Norristown

PA USA

Cousins AW SAAO Circ

ESA The Hipparcos and Tycho Catalogues ESA SP

Jenkner H Lasker B Sturch C McLean B Shara M Russell J AJ

Kwee KK van Woerden H BAN

Robb RM Greimel R Ouellette J IBVS No

Rob ertson TH and Hamilton JE AJ

Stephenson CB AJ