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A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Information Bulletin on Variable Stars
COMMISSIONS AND OF THE I A U INFORMATION BULLETIN ON VARIABLE STARS Nos November July EDITORS L SZABADOS K OLAH TECHNICAL EDITOR A HOLL TYPESETTING K ORI ADMINISTRATION Zs KOVARI EDITORIAL BOARD L A BALONA M BREGER E BUDDING M deGROOT E GUINAN D S HALL P HARMANEC M JERZYKIEWICZ K C LEUNG M RODONO N N SAMUS J SMAK C STERKEN Chair H BUDAPEST XI I Box HUNGARY URL httpwwwkonkolyhuIBVSIBVShtml HU ISSN 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 means electronic or otherwise without the prior written p ermission of the publishers Prior written p ermission of the publishers is required for entering IBVS issues to an electronic indexing or bibliographic system to o CONTENTS C STERKEN A JONES B VOS I ZEGELAAR AM van GENDEREN M de GROOT On the Cyclicity of the S Dor Phases in AG Carinae ::::::::::::::::::::::::::::::::::::::::::::::::::: : J BOROVICKA L SAROUNOVA The Period and Lightcurve of NSV ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::: W LILLER AF JONES A New Very Long Period Variable Star in Norma ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::::: EA KARITSKAYA VP GORANSKIJ Unusual Fading of V Cygni Cyg X in Early November ::::::::::::::::::::::::::::::::::::::: -
121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S. -
Astronomical Coordinate Systems
Appendix 1 Astronomical Coordinate Systems A basic requirement for studying the heavens is being able to determine where in the sky things are located. To specify sky positions, astronomers have developed several coordinate systems. Each sys- tem uses a coordinate grid projected on the celestial sphere, which is similar to the geographic coor- dinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth’s equator). Each coordinate system is named for its choice of fundamental plane. The Equatorial Coordinate System The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the most closely related to the geographic coordinate system because they use the same funda- mental plane and poles. The projection of the Earth’s equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles onto the celestial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate sys- tems: the geographic system is fixed to the Earth and rotates as the Earth does. The Equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but it’s really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec. for short). It measures the angle of an object above or below the celestial equator. -
Binocular Universe: Aurigan Treasures
Binocular Universe: Aurigan Treasures February 2012 Phil Harrington ead outside this evening and take a look high overhead. If you live in midnorthern latitudes, you will find a lone beacon cresting near the zenith as Hthe sky darkens. That's Capella, the Alpha (α) star of the constellation Auriga the Charioteer. Tracing back to ancient Rome, the name Capella translates as "She-Goat," a reference to the position it holds in the picture of the Charioteer. He is often portrayed as holding a goat and two kids in his arms. Above: Winter star map from Star Watch by Phil Harrington. Finder chart for this month's Binocular Universe, adapted from TUBA, www.philharrington.net/tuba.htm Today, we know that Capella is actually a binary star system lying some 42 light years away. Each of Capella's suns is classified as a type-G yellow star, like our Sun. That means that all three have roughly the same surface temperature, although our yellow dwarf Sun is only about one-tenth as large as either of the Capella giants. There is little hope of spotting the two Capella component stars through even the largest telescopes, since they are only separated by about 60 million miles, less than the distance from the Sun to Venus. The Charioteer’s pentagonal body highlights a wonderful area of the winter sky to scan with binoculars. There, you will find three of the season’s brightest open star clusters as well as an array of lesser known targets. M38, one of Auriga's three Messier open clusters, is centrally positioned within Auriga’s pentagonal body. -
Information Bulletin on Variable Stars
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 means electronic or otherwise without the prior written p ermission of the publishers 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 ::::::::::::::::::::::::::::::::::::::::::::::::::: -
Flare Stars Across the HR Diagram
Journal of Integrated Creative Studies Flare stars across the H-R diagram Luis A. Balona1 1South African Astronomical Observatory E-mail: [email protected] Abstract. Flare stars appear to be as common among the hottest stars as among the coolest. Starspots, which are closely associated with flares, are likewise common among stars of all spectral types. This finding contradicts the long-help belief that only stars with convective envelopes can sustain magnetic fields. It is found that rotation is a dominant factor in inducing flares: flare stars nearly always have shorter rotation periods than non-flare stars. These findings have important implications for the atmospheres of A and B stars as well as providing clues for the formation of the corona. Keywords: Stars: flare, Stars: activity 1. Workshop on stars with superflares I attended the Workshop on Superflares on Solar-type stars and Solar flares in which I was invited to give a talk. I am grateful to Professor Shibata for the opportunity to interact with the Superflare group of Kyoto University who originally discovered superflares in the data from the Kepler spacecraft and are recognized as leading researchers in this field. The meeting was also attended by internationally renowned researchers on flare stars who contributed excellent talks and stimulated lively discussions. I thank Professor Shibata and his group for organizing such a productive workshop. 2. Stellar activity across the H-R diagram It is accepted that stellar magnetic fields are either of fossil origin (the star was born with the magnetic field already present) or are generated by convection in accordance with the dynamo theory. -
Almanacco Astronomico 2002 – Introduzione
Almanacco Astronomico per l’anno 2002 Sergio Alessandrelli C.C.C.D.S. - Hipparcos La Luna – Principali formazioni geologiche Almanacco Astronomico per l’anno 2002 A tutti gli amici astrofili… 1 Almanacco Astronomico 2002 – Introduzione Introduzione all’Almanacco Astronomico 2002 Il presente Almanacco Astronomico è stato realizzato utilizzando comuni programmi di calcolo astronomico facilmente reperibili sul mercato del software, ovvero scaricabili gratuitamente tramite Internet. La precisione nei calcoli è quindi quella tipica per questo tipo di software, ossia sufficiente per gli usi dell’astrofilo medio. Tutti gli eventi sono stati calcolati per le coordinate di Roma (Lat. 41° 52’ 48” N, Long. 12° 30’ 00” E) e gli orari espressi (tranne laddove altrimenti specificato) in tempo universale. 2 Almanacco Astronomico 2002 – Calendario del 2002 Calendario del 2002 January February March Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa 1 2 3 4 5 1 2 1 2 6 7 8 9 10 11 12 3 4 5 6 7 8 9 3 4 5 6 7 8 9 13 14 15 16 17 18 19 10 11 12 13 14 15 16 10 11 12 13 14 15 16 20 21 22 23 24 25 26 17 18 19 20 21 22 23 17 18 19 20 21 22 23 27 28 29 30 31 24 25 26 27 28 24 25 26 27 28 29 30 31 April May June Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa Su Mo Tu We Th Fr Sa 1 2 3 4 5 6 1 2 3 4 1 7 8 9 10 11 12 13 5 6 7 8 9 10 11 2 3 4 5 6 7 8 14 15 16 17 18 19 20 12 13 14 15 16 17 18 9 10 11 12 13 14 15 21 22 23 24 25 26 27 19 20 21 22 23 24 25 16 17 18 19 20 21 22 28 29 30 26 27 28 29 30 31 23 24 25 26 27 28 29 30 July August September Su Mo Tu We -
Low Mass Star Formation in Southern Molecular Clouds
•A •• No. 11 - November 1991 Low Mass Star Formation in Southern Molecular Clouds Edited by Ba Reipurth Published by EUROPEAN SOUTHERN OBSERVATORY Karl-Schwarzschild-Straße 2, D-8046 Garching bei München Germany © Copyright ESO 1992 Low Mass Star Formation in Southern Molecular Clouds Edited by Bo Reipurth ESO Scientific Report No. 11 November 1991 Table of Contents Low Mass Star Formation in Orion 1 J. Brand and J.G.A. Wouterloot The Canis Majoris OBl Association 59 G.lT. IIerbig Low Mass Star Formation in Puppis and Vela 69 B. Pcttcrsson The Chamaeleon Dark Clouds and T-Associations 93 R.D. Schu'artz The Southern Coalsack - Where are a11 the Young Stars? 119 L.-A Nyman The Star Forming Region in Lupus 127 J. Kraulter Young Low Mass Stars in the Norma Cloud 149 B. Reipurth and J.A. Graham Star Formation in the Ophiuchus Molecular Cloud Complex 159 B.A. lVilking Star Formation in the Corona Australis Region 185 J.A. Graham The Serpens Molecular Cloud 197 C. Eiroa iii Foreword and Acknowledgements In July 1989 an ESO Workshop on "Low Mass Star 'Formation and Pre-Main Sequence Objects" was held in Garehing near Munieh, Germany. The papers presented were published as ESO Conference and Workshop Proceedings No. 33. As part of the scientific activities of the workshop, a special poster session was held in which all the major southern star forming regions were described one by one by researchers with extensive experience in each. The purpose of this mini poster session was to attract attention to the richness of the southern star forming regions. -
X-Rays from Low and Intermediate Mass Stars
X-rays from low and intermediate mass stars Jan Robrade Hamburger Sternwarte X-ray Universe, Dublin, 16-19 June 2014 The solar corona Sun in X-rays: SDO, Yohkoh, TRACE Solar corona is highly structured and dynamic Jan Robrade (Hamburger Sternwarte) X-rays from Stars 16.06.2014 2 / 23 Stellar X-ray emission This talk: Low and intermediate mass stars X-ray generation mechanisms Time evolution of X-ray emission ’The X-ray HRD’ (G¨udel 2004) X-ray stars are (virtually) everywhere! Jan Robrade (Hamburger Sternwarte) X-rays from Stars 16.06.2014 3 / 23 Cool stars in X-rays The solar neighborhood: volume limited (Schmitt 1997) X-ray surface flux varies by orders of magnitude at given B-V Sun weakly active, coronal holes describe lower limit X-ray activity declines towards hotter stars Jan Robrade (Hamburger Sternwarte) X-rays from Stars 16.06.2014 4 / 23 Cool stars in X-rays Activity-dynamo relation (F - mid M) (Wright+ 2011) X-rays from magnetic activity, log LX/Lbol ≈ −3 ... −7 LX ∝ dynamo power; Ro = P/τc powerlaw (slope?) - saturation (level, breakpoint ?) - supersaturation (?) Jan Robrade (Hamburger Sternwarte) X-rays from Stars 16.06.2014 4 / 23 Coronal dynamo regimes Activity regimes of stars (blue: Ro = 0.13, red: Rc /R∗ = 3, green: GX = 0.01) (Wright+ 2011) (also: Jeffries+ 2011) dynamo regimes depend on mass and rotation supersaturation: excess polar updraft vs. centrifugal stripping Jan Robrade (Hamburger Sternwarte) X-rays from Stars 16.06.2014 5 / 23 X-ray activity at very low masses Very red dwarfs are faint.. -
Chromospheric and Coronal Activity in Solar-Like Stars
Chromospheric and coronal activity in solar-like stars Dissertation zur Erlangung des Doktorgrades des Departments Physik der Universitat¨ Hamburg vorgelegt von Christian Schroder¨ geboren in Hamburg Hamburg 2008 ii Gutachter der Dissertation: Prof. J.H.M.M. Schmitt Dr. Ansgar Reiners Gutachter der Disputation: Prof. J.H.M.M. Schmitt Prof. P.H. Hauschildt Datum der Disputation: 18.07.2008 Vorsitzender des Pr¨ufungsausschusses: Prof. G. Wiedemann Vorsitzender des Promotionsausschusses: Prof. J. Bartels Dekan der Fakult¨at f¨ur Mathematik, Informatik und Naturwissenschaften: Prof. Dr. Arno Fr¨uhwald iv Zusammenfassung Der Begriff ”stellare Aktivit¨at” fasst diverse Ph¨anomene auf der Sternenoberfl¨ache und in der Stern- atmosph¨are zusammen. Die Ursache f¨ur diese Ph¨anomene sind Ver¨anderungen in den Magnetfeldern der Sterne. W¨ahrend es bei der Sonne m¨oglich ist, die verschiedenen Formen der Aktivit¨at direkt und detailliert zu beobachten, ist dies bei anderen Sternen nicht m¨oglich. Durch eine genaue Analyse der Spektren von Sternen lassen sich dennoch Informationen ¨uber deren Aktivit¨at gewinnen. Die folgende Arbeit befasst sich mit zwei Arten der stellaren Aktivit¨at: zum einen mit der R¨ontgenaktivit¨at von Sternen des Spektraltyps A und ihrer potentiellen Ursache, zum zweiten mit der chromosph¨arischen Aktivit¨at von Sternen im Bereich der sp¨aten A- bis sp¨aten K-Sterne. Da im Bereich der sp¨aten A- bis fr¨uhen F-Sterne der Dynamo, der f¨ur die Aktivit¨at in sonnen¨ahnlichen Sternen verant- wortlich ist, entsteht, ist dieser Spektralbereich f¨ur das Verst¨andnis der stellaren Aktivit¨at von besonderer Bedeutung. -
New X-Ray Observations of IQ Aurigae and Α2 Canum Venaticorum Probing the Magnetically Channeled Wind Shock Model in A0p Stars J
A&A 531, A58 (2011) Astronomy DOI: 10.1051/0004-6361/201116843 & c ESO 2011 Astrophysics New X-ray observations of IQ Aurigae and α2 Canum Venaticorum Probing the magnetically channeled wind shock model in A0p stars J. Robrade and J. H. M. M. Schmitt Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany e-mail: [email protected] Received 7 March 2011 / Accepted 11 May 2011 ABSTRACT Aims. We re-examine the scenario of X-ray emission from magnetically confined/channeled wind shocks (MCWS) for Ap/Bp stars, a model originally developed to explain the ROSAT detection of the A0p star IQ Aur. Methods. We present new X-ray observations of the A0p stars α2 CVn (Chandra)andIQAur(XMM-Newton) and discuss our findings in the context of X-ray generating mechanisms of magnetic, chemically peculiar intermediate mass stars. −1 2 −1 Results. The X-ray luminosities of IQ Aur with log LX = 29.6ergs and α CVn with log LX 26.0ergs differ by at least three orders of magnitude, although both are A0p stars. By studying a sample of comparison stars, we find that X-ray emission is preferably generated by more massive objects such as IQ Aur. Besides a strong, cool plasma component, significant amounts of hot (>10 MK) plasma are present during the quasi-quiescent phase of IQ Aur; moreover, diagnostics of the UV sensitive f /i line ratio in He-like O vii triplet point to X-ray emitting regions well above the stellar surface of IQ Aur. In addition we detect a large flare from IQ Aur −1 with temperatures up to ∼100 MK and a peak X-ray luminosity of log LX ≈ 31.5ergs .