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COMMISSION 27 OF THE I.A.U.
INFORMATION BULLETIN ON VARIABLE STARS

Nos. 2401 - 2500
1983 September - 1984 March

EDITORS: B. SZEIDL AND L. SZABADOS, KONKOLY OBSERVATORY
1525 BUDAPEST, Box 67, HUNGARY
HU ISSN 0374-0676
CONTENTS 2401 A POSSIBLE CATACLYSMIC VARIABLE IN CANCER
Masaaki Huruhata 20 September 1983

2402 A NEW RR-TYPE VARIABLE IN LEO
Masaaki Huruhata 20 September 1983

2403 ON THE DELTA SCUTI STAR BD +43d1894
A. Yamasaki, A. Okazaki, M. Kitamura 23 September 1983

2404 IQ Vel: IMPROVED LIGHT-CURVE PARAMETERS
L. Kohoutek 26 September 1983

2405 FLARE ACTIVITY OF EPSILON AURIGAE?
I.-S. Nha, S.J. Lee 28 September 1983

2406 PHOTOELECTRIC OBSERVATIONS OF 20 CVn
Y.W. Chun, Y.S. Lee, I.-S. Nha 30 September 1983

2407 MINIMUM TIMES OF THE ECLIPSING VARIABLES AH Cep AND IU Aur
Pavel Mayer, J. Tremko 4 October 1983

2408 PHOTOELECTRIC OBSERVATIONS OF THE FLARE STAR EV Lac IN 1980
G. Asteriadis, S. Avgoloupis, L.N. Mavridis, P. Varvoglis 6 October 1983

2409 HD 37824: A NEW VARIABLE STAR
Douglas S. Hall, G.W. Henry, H. Louth, T.R. Renner 10 October 1983

2410 ON THE PERIOD OF BW VULPECULAE
E. Szuszkiewicz, S. Ratajczyk 12 October 1983

2411 THE UNIQUE DOUBLE-MODE CEPHEID CO Aur
E. Antonello, L. Mantegazza 14 October 1983

2412 FLARE STARS IN TAURUS
A.S. Hojaev 14 October 1983

2413 BVRI PHOTOMETRY OF THE ECLIPSING BINARY QX Cas
Thomas J. Moffett, T.G. Barnes, III 17 October 1983

2414 THE ABSOLUTE MAGNITUDE OF AZ CANCRI
William P. Bidelman, D. Hoffleit 17 October 1983

2415 NEW DATA ABOUT THE APSIDAL MOTION IN THE SYSTEM OF RU MONOCEROTIS
D.Ya. Martynov 18 October 1983

2416 V LIGHT CURVE OF CC COMAE
G.V. Zhukov 18 October 1983

2417 SPECTROSCOPIC INVESTIGATION OF SZ Lyn AND SS Psc
G.A. Garbuzov 18 October 1983

2418 INACTIVE STATE OF MV LYRAE
I.L. Andronov, S.Yu. Shugarov 18 October 1983

2419 HD 34409 - A DELTA SCUTI VARIABLE
R.K. Srivastava, A.K. Arya 19 October 1983

2420 TWO NEW VARIABLE STARS IN THE FIELD OF NGC 6946
G. Romano, M. Perissinotto 19 October 1983

2421 NOTE OF THE SEMI-REGULAR VARIABLE TT Scl
P.S. The 24 October 1983

2422 FT LUPI: STUDY OF THE PERIOD AND LIGHT CURVE
S.L. Lipari, R.F. Sistero 24 October 1983

2423 V1057 CYGNI
Gunnar Welin 25 October 1983

2424 PHOTOELECTRIC MINIMA TIMES OF BX ANDROMEDAE
P. Rovithis, H. Rovithis-Livaniou 1 November 1983

2425 DETERMINATION OF CEPHEID DISTANCES BY MEANS OF WESENHEIT FUNCTION
Antoni Opolski 1 November 1983

2426 AD Leo FLARE MONITORING
Richard B. Herr, J.D. Frank 2 November 1983

2427 PHOTOELECTRIC HalphaW OBSERVATIONS OF R CMa
M.T. Edalati, B. Khalesse, N. Riazi 2 November 1983

2428 NEW OBSERVATIONS OF HZ Her
V.V. Hambarian, G.H. Broutian CORRIGENDUM 8 November 1983

2429 PHOTOMETRIC STUDY OF IO ANDROMEDAE
I.L. Andronov 9 November 1983

2430 ON THE CYCLE LENGTH OF THE CATACLYSMIC VARIABLE T LEONIS
W. Wenzel 9 November 1983
2431 SUDDEN BRIGHTENING OF THE RECENTLY DISCOVERED Be STAR HR 7739
K. Pavlovski, H. Bozic, P. Harmanec, J. Horn, P. Koubsky 14 November 1983

2432 POLARIMETRY OF Be STARS IN THE OPEN CLUSTER NGC 6611
L.A.S. Reis, E. Janot-Pachecho 18 November 1983

2433 A NEW PROBABLE FLARE STAR
N. Sanduleak 23 November 1983

2434 ANOTHER SEMI-REGULAR VARIABLE IN CYGNUS
G. Auner, H. Hartl, R. Weinberger 25 November 1983

2435 ON THE VARIABILITY OF THE STAR SAO 072799
P.G. Niarchos 25 November 1983

2436 ON THE PERIOD OF BD Cir
Silvano F. Marton, A. Grieco 28 November 1983

2437 PHOTOELECTRIC OBSERVATIONS OF UV CETI
M.K. Tsvetkov, L.N. Mavridis, G.A. Asteriadis 29 November 1983

2438 PERIODIC LIGHT VARIABILITY OF PG1711+336
A.V. Mironov, V.G. Moshkalev, S.Yu. Shugarov 30 November 1983

2439 V417 AQUILAE: PHOTOELECTRIC OBSERVATIONS AND IMPROVED PERIOD
Danny R. Faulkner 2 December 1983

2440 V3876 Sgr, A MIRA STAR, NOT A NOVA
Emilia P. Belserene 5 December 1983

2441 PHOTOMETRIC VARIATIONS IN THE Ap STAR HD 215441
M. Corbin 5 December 1983

2442 PHOTOELECTRIC OBSERVATIONS OF R CrB
D. Bohme 9 December 1983

2443 REMARKS ON THREE VARIABLE STARS
Thomas Berthold 9 December 1983

2444 EPSILON AURIGAE
Eugenio E. Mendoza V. 13 December 1983

2445 POLARIMETRIC OBSERVATIONS OF Be STARS
L.A.S. Reis, E. Janot-Pachecho 14 December 1983
2446 THE HBeta EMISSION OF PU Vul
Liu Zongli, Hao Xiangliang 16 December 1983

2447 THE Be BINARY HR 2142: NO 0.13m BRIGHTNESS DECREASE IN JANUARY 1983
P. Harmanec, J. Horn, P. Koubsky, K. Pavlovski, H. Bozic, J. Ziznovsky, J.R. Percy 16 December 1983

2448 A NOTE ON X TRIANGULI
P. Rovithis, H. Rovithis-Livaniou 20 December 1983

2449 X-RAY VARIABLE STARS IN THE PLEIADES
S. Sciortino, G. Micela, S. Serio, G.S. Vaiana, L. Golub, F.R. Harnden, Jr., R. Rosner 20 December 1983

2450 FLARE LIKE ACTIVITY IN AR LACERTAE
R.K. Srivastava 23 December 1983

2451 PHOTOELECTRIC TIMES OF MINIMA OF ECLIPSING VARIABLES
P.G. Niarchos 23 December 1983

2452 ACTIVE AND INACTIVE STATES OF THE X-RAY BINARY 4U 2129+47 =
V1727 CYGNI W. Wenzel 27 December 1983

2453 VARIABLE STAR TIMINGS FROM ARIZONA
Andrew P. Odell, F. Dorchak, K. Rogalski, S. Tapia, W.Z. Wisniewski, D.H. Smith 27 December 1983

2454 HD 104901B AN F-TYPE SUPERGIANT ECLIPSING BINARY
Olin J. Eggen 28 December 1983

2455 Halpha VARIABILITY IN ALPHA LYRAE
P.S. Goraya, M. Singh 30 December 1983

2456 CO Aur - DOUBLE MODE CHARACTER CONFIRMED
B. Fuhrmann, R.H. Schult 2 January 1984

2457 NEW PHOTOELECTRIC MINIMA TIMES OF VW CEPHEI
P. Rovithis, H. Rovithis-Livaniou 4 January 1984

2458 A DATABASE FOR RS CVn BINARY STAR SYSTEMS
E. Nelson, M. Zeilik 6 January 1984

2459 THE LONG TIME BEHAVIOUR OF THE POLAR AM Her IN 1983
W. Gotz 10 January 1984

2460 ON THE DELTA SCUTI-LIKE VARIABILITY OF THE Ap STAR HD 10088
Tobias J. Kreidl 16 January 1984
2461 THE LIGHT CURVE OF FG Vul IN 1983
W. Gotz 18 January 1984

2462 ON THE SX Phe-TYPE STARS
M.S. Frolov, B.N. Irkaev 20 January 1984

2463 NEW DATA ON THE MOST RECENT MINIMUM OF THE X-RAY SOURCE KR Aur
Martha H. Liller, M.D. Popova 20 January 1984

2464 REVISED PHOTOMETRIC RESULTS OF SAO 072799
P.G. Niarchos 24 January 1984

2465 NARROW BAND PHOTOMETRY OF FG Vir
P. Lopez de Coca, R. Garrido, V. Costa, A. Rolland 27 January 1984

2466 WEAKENING OF HBeta EMISSION OF PU Vul
Liu Zongli, Hao Xiangliang 30 January 1984

2467 FURTHER OBSERVATIONS OF THE CENTRAL STAR IN THE PLANETARY NEBULA
NGC 2346 Brian F. Marino, H.O. Williams, W.S.G. Walker 1 February 1984

2468 THE ORBITAL PERIOD AND PHOTOGRAPHIC LIGHT CURVE OF THE ECLIPSING BINARY
V339 Per E.H. Geyer, F. Gieseking 3 February 1984

2469 PERIOD CHANGE OF THE ECLIPSING BINARY IM AURIGAE
O. Gulmen, C. Sezer, N. Gudur 6 February 1984

2470 OUTBURST OF VY Aqr IN 1983
Masaaki Huruhata 6 February 1984

2471 POSSIBLE DISCOVERY OF REPEATING OSCILLATIONS IN THE BRIGHTNESS OF
BY DRACONIS ON TIMESCALES OF 1-3 HOURS P.F. Chugainov 7 February 1984

2472 LACK OF DETECTION OF A 1.77 h -PERIODICITY IN THE CP STAR HD 32633
Tobias J. Kreidl 8 February 1984

2473 EPOCHS OF MINIMUM LIGHT, DISPLACED SECONDARY ECLIPSE OF SW LACERTAE
Danny R. Faulkner, E.E. Evans III, D.H. Grossoehme, E.J. Moyer, Jr. 8 February 1984

2474 NEW OBSERVATIONS OF CN ANDROMEDAE
E.J. Michaels, N.L. Markworth, J.B. Rafert 8 February 1984

2475 PERIODIC LIGHT CURVE VARIATIONS OF RT LACERTAE
S. Evren, C. Ibanoglu, Z. Tunca, O. Tumer 9 February 1984

2476 NEW VARIABLE STARS IN THE Gamma CYGNI REGION
Katya P. Tsvetkova 10 February 1984

2477 ON THE PERIOD OF BH CENTAURI
Tibor J. Herczeg 13 February 1984

2478 ON THE PERIODS OFF RZ COMAE AND V1073 CYGNI
Zeki Aslan, T.J. Herczeg 13 February 1984

2479 ON THE PERIOD OF THE W UMa SYSTEM Epsilon CrA
J. Manfroid, M. Lunel, J. Bergeat, P. Bouchet 15 February 1984

2480 THE PHASE BEHAVIOUR OF THE GENEVA Z AND DELTA(V1-G) PARAMETERS FOR
41 Tau, 56 Tau AND 49 Cnc M. Muciek, J. Gertner, P. North, F.G. Rufener 17 February 1984

2481 ON THE NATURE OF THE CATACLYSMIC BINARY V2051 OPHIUCHI
W. Wenzel 22 February 1984

2482 A FLARE-LIKE EVENT ON THE LIGHT CURVE OF V351 Ori
G.U. Kovalchuk 24 February 1984

2483 FO And - PROBABLY A NEW MEMBER OF THE SU UMa SUB-GROUP OF DWARF NOVAE
L. Meinunger 29 February 1984

2484 PHOTOELECTRIC OBSERVATIONS OF THE FLARE STAR UV Cet IN OCTOBER 1983
I.V. Ilyin 1 March 1984

2485 THE ECLIPSE OF THE SYMBIOTIC ECLIPSING BINARY SYSTEM CI CYGNI IN 1982
T.S. Belyakina 5 March 1984

2486 THE DISCOVERY OF A W URSAE MAJORIS VARIABLE IN THE VISUAL BINARY SYSTEM ADS 9019
R.L. Walker 6 March 1984

2487 PHOTOELECTRIC OBSERVATIONS OF THE EW-VARIABLE VZ Psc
E. Poretti 6 March 1984

2488 IMPROVED POSITIONS FOR 15 CATACLYSMIC VARIABLE STARS
Alan L. Kiplinger 7 March 1984

2489 NEW DOUBLE-LINED ECLIPSING BINARIES FOUND WITH RETICON, DIGICON, AND
CCD DETECTORS Claud H. Lacy 7 March 1984
2490 IMPROVED OUTBURST LIGHT CURVES OF THE NOVAE EY Aql, BC Cas, MT Cen,
AND V745 Sco H.W. Duerbeck 7 March 1984

2491 HIGHLY EXCITED EMISSION LINES IN BX Mon AND ZZ CMi
T. Iijima 13 March 1984

2492 A CLOSE ECLIPSING BINARY SYSTEM IN CYGNUS
S.Yu. Shugarov 16 March 1984

2493 SHELL EPISODE OF PLEIONE (BU Tau)
P.S. Goraya 19 March 1984

2494 BD +37d443: A NON-VARIABLE STAR
Andrea Cimatti, M. Lolli, G. Mengoli 21 March 1984

2495 ON THE PERIOD OF AG PEGASI
R. Luthardt 22 March 1984

2496 AN UV ACTIVE PHENOMENON OF EPSILON AURIGAE
Tosio Oki, I. Sekiya, K. Hirayama 23 March 1984

2497 NEW LIGHT ELEMENTS AND TIMES OF MINIMUM FOR AO CAMELOPARDALIS
Ernest E. Evans III, D.H. Grossoehme, E.J. Moyer, Jr. 23 March 1984

2498 SIX NEW VARIABLE STARS
H.H. Guetter, A.V. Hewitt 28 March 1984

2499 UBV OBSERVATIONS FOR ELEVEN KNOWN VARIABLE STARS
H.H. Guetter, A.V. Hewitt 28 March 1984

2500 PHOTOELECTRIC OBSERVATIONS OF CY AQUARII
A. Purgathofer, A. Schnell 28 March 1984

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    Absolute-Magnitude Calibration for W Uma-Type Systems. II. in Uence Of

    AbsoluteMagnitude Calibration for W UMatype Systems I I Inuence of Metallicity 1 Slavek Rucinski Longb ow Drive Scarb orough Ontario MW W Canada March ABSTRACT A mo dication to the absolute magnitude calibration for W UMatype systems taking into account dierences in metal abundances is derived on the basis of contact binary systems recently discovered in metalp o or clusters A preliminary estimate of the magnitude of the metallicitydependent term for the B V based calibration is M F eH The calibration based on the V I color is V C exp ected to b e less sensitive with the correction term F eH Need for a metallicitydependent term in the calibration Searches for gravitational microlenses are currently giving large numbers of serendipitously discovered variable stars Among these variables there are many W UMatype contact binaries On the basis of the rst part of the catalog of variable stars discovered during the OGLE pro ject Udalski et al one can estimate the total number of contact binaries which will b e discovered in the Baade Window during OGLE at well over one thousand This estimate is based on discoveries of such systems in the rst part of the catalog which covered one of the OGLE elds ie less than of the whole area searched the Central Baade Window BWC and reached I The newly discovered systems will provide excellent statistics for the p erio d color and amplitude distributions of contact binaries much b etter than those based on the skyeld sample which is heavily biased towards largeamplitude variables Kaluzny
  • Cfa in the News ~ Week Ending 3 January 2010

    Cfa in the News ~ Week Ending 3 January 2010

    Wolbach Library: CfA in the News ~ Week ending 3 January 2010 1. New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 2. 2009 in science and medicine, ROGER SCHLUETER, Belleville News Democrat (IL), Sunday, January 3, 2010 3. 'Science, celestial bodies have always inspired humankind', Staff Correspondent, Hindu (India), Tuesday, December 29, 2009 4. Why is Carpenter defending scientists?, The Morning Call, Morning Call (Allentown, PA), FIRST ed, pA25, Sunday, December 27, 2009 5. CORRECTIONS, OPINION BY RYAN FINLEY, ARIZONA DAILY STAR, Arizona Daily Star (AZ), FINAL ed, pA2, Saturday, December 19, 2009 6. We see a 'Super-Earth', TOM BEAL; TOM BEAL, ARIZONA DAILY STAR, Arizona Daily Star, (AZ), FINAL ed, pA1, Thursday, December 17, 2009 Record - 1 DIALOG(R) New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 TEXT: "In this paper we report on testing the 'rolen model' and 'opportunity-structure' hypotheses about the parents whom scientists mentioned as career influencers. According to the role-model hypothesis, the gender match between scientist and influencer is paramount (for example, women scientists would disproportionately often mention their mothers as career influencers)," scientists writing in the journal Social Studies of Science report (see also ). "According to the opportunity-structure hypothesis, the parent's educational level predicts his/her probability of being mentioned as a career influencer (that ism parents with higher educational levels would be more likely to be named). The examination of a sample of American scientists who had received prestigious postdoctoral fellowships resulted in rejecting the role-model hypothesis and corroborating the opportunity-structure hypothesis.
  • PHAS 1102 Physics of the Universe 3 – Magnitudes and Distances

    PHAS 1102 Physics of the Universe 3 – Magnitudes and Distances

    PHAS 1102 Physics of the Universe 3 – Magnitudes and distances Brightness of Stars • Luminosity – amount of energy emitted per second – not the same as how much we observe! • We observe a star’s apparent brightness – Depends on: • luminosity • distance – Brightness decreases as 1/r2 (as distance r increases) • other dimming effects – dust between us & star Defining magnitudes (1) Thus Pogson formalised the magnitude scale for brightness. This is the brightness that a star appears to have on the sky, thus it is referred to as apparent magnitude. Also – this is the brightness as it appears in our eyes. Our eyes have their own response to light, i.e. they act as a kind of filter, sensitive over a certain wavelength range. This filter is called the visual band and is centred on ~5500 Angstroms. Thus these are apparent visual magnitudes, mv Related to flux, i.e. energy received per unit area per unit time Defining magnitudes (2) For example, if star A has mv=1 and star B has mv=6, then 5 mV(B)-mV(A)=5 and their flux ratio fA/fB = 100 = 2.512 100 = 2.512mv(B)-mv(A) where !mV=1 corresponds to a flux ratio of 1001/5 = 2.512 1 flux(arbitrary units) 1 6 apparent visual magnitude, mv From flux to magnitude So if you know the magnitudes of two stars, you can calculate mv(B)-mv(A) the ratio of their fluxes using fA/fB = 2.512 Conversely, if you know their flux ratio, you can calculate the difference in magnitudes since: 2.512 = 1001/5 log (f /f ) = [m (B)-m (A)] log 2.512 10 A B V V 10 = 102/5 = 101/2.5 mV(B)-mV(A) = !mV = 2.5 log10(fA/fB) To calculate a star’s apparent visual magnitude itself, you need to know the flux for an object at mV=0, then: mS - 0 = mS = 2.5 log10(f0) - 2.5 log10(fS) => mS = - 2.5 log10(fS) + C where C is a constant (‘zero-point’), i.e.
  • Variable Star Section Circular

    Variable Star Section Circular

    ΒΑΛ The British Astronomical Association VARIABLE STAR SECTION CIRCULAR 64 "LIGHT-CURVE” AUGUST 1986 ISSN 0267-9272 Office: Burlington House, Piccadilly, London, W1V 9AG SECTION OFFICERS: Director D.R.B. Saw, 'Upanova1, 18 Dolllcott, Haddenham, Aylesbury, Bucks. HP17 8JG Tel: Haddenham (0844) 292065 Assistant Director S.R. Dunlop, 140 Stocks Lane, East Wittering, nr Chichester, West Sussex P020 8NT Tel: Bracklesham Bay (0243) 670354 Secretary M.D. Taylor, 17 Cross Lane, Wakefield, West Yorkshire WF2 8DA Tel: Wakefield (0924) 374651 Programme Secretaries: Assistant Secretary (Post temporarily vacant) Telescopic Assistant Secretary J. Toone, 2 Hilton Crescent, Boothstown, Binocular Worsley, Manchester M28 4FY Tel: 061 702 8619 Eclipsing Binary J.E. Isles, Rose Cottage, 22 High Street, Secretary Wescott, Bucks. HP18 OPU Tel: Aylesbury (0296) 651779 Nova/Supernova G.M Hurst, 16 Westminster Close, Search Secretary Kempshott Rise, Basingstoke, Hants. RG22 4PP Tel: Basingstoke (0256) 471074 Chart Secretary J. Parkinson, 229 Scar Lane, Golcar, (except Eclipsing) Huddersfield, West Yorkshire HD7 4AU Tel: Huddersfield (0484) 642947 For subcription rates and charges for charts and other publications see inside back cover. Editorial It has been suggested that these C irc u la rs are often a little 'dry' and technical for some members. We are always happy to receive more 'personal' items and hope to include more in future issues. We are also including an occasional short note on some of the terms encountered, and which may not be fully explained in some of the specific articles. The first such item appears on p.13. If you have any queries, however elementary, please send them in, and we shall do our best to provide the answers.