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Arxiv:Astro-Ph/0204354 V1 20 Apr 2002 1 DI Ilb Netdb Adlater) Hand by Inserted Be Will (DOI: Astrophysics & Astronomy H Uecn Dnicto Fi O a Confusing
Astronomy & Astrophysics manuscript no. June 3, 2005 (DOI: will be inserted by hand later) Recurrent Nova IM Normae Taichi Kato1, Hitoshi Yamaoka2, William Liller3, and Berto Monard4 1 Department of Astronomy, Kyoto University, Kyoto 606-8502, Japan 2 Faculty of Science, Kyushu University, Fukuoka 810-8560, Japan 3 Center for Nova Studies, Casilla 5022 Renaca, Vi˜na del Mar, Chile 4 Bronberg Observatory, PO Box 11426, Tiegerpoort 0056, South Africa Received / accepted Abstract. We detected the second historical outburst of the 1920 nova IM Nor. Accurate astrometry of the outbursting object revealed the true quiescent counterpart having a magnitude of R=17.0 mag and B=18.0 mag. We show that the quiescent counterpart shows a noticeable variation. From the comparison of light curves and spectroscopic signatures, we propose that IM Nor and CI Aql comprise a new class of recurrent novae bearing some characteristics similar to those of classical novae. We interpret that the noticeable quiescent variation can be a result of either high orbital inclination, which may be also responsible for the low quiescent brightness, or the presence of high/low states. If the second possibility is confirmed by future observations, IM Nor becomes the first recurrent nova showing state changes in quiescence. Such state changes may provide a missing link between recurrent novae and supersoft X-ray sources. Key words. novae, cataclysmic variables — Stars: individual (IM Nor) 1. Introduction nal studies, Duerbeck (1987) reported the remeasured po- sition of the nova, and different candidates for the qui- IM Nor was originally discovered as a possible nova in 1920 escent counterpart, whose exact identification remained by I. -
Pulsating Components in Binary and Multiple Stellar Systems---A
Research in Astron. & Astrophys. Vol.15 (2015) No.?, 000–000 (Last modified: — December 6, 2014; 10:26 ) Research in Astronomy and Astrophysics Pulsating Components in Binary and Multiple Stellar Systems — A Catalog of Oscillating Binaries ∗ A.-Y. Zhou National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; [email protected] Abstract We present an up-to-date catalog of pulsating binaries, i.e. the binary and multiple stellar systems containing pulsating components, along with a statistics on them. Compared to the earlier compilation by Soydugan et al.(2006a) of 25 δ Scuti-type ‘oscillating Algol-type eclipsing binaries’ (oEA), the recent col- lection of 74 oEA by Liakos et al.(2012), and the collection of Cepheids in binaries by Szabados (2003a), the numbers and types of pulsating variables in binaries are now extended. The total numbers of pulsating binary/multiple stellar systems have increased to be 515 as of 2014 October 26, among which 262+ are oscillating eclipsing binaries and the oEA containing δ Scuti componentsare updated to be 96. The catalog is intended to be a collection of various pulsating binary stars across the Hertzsprung-Russell diagram. We reviewed the open questions, advances and prospects connecting pulsation/oscillation and binarity. The observational implication of binary systems with pulsating components, to stellar evolution theories is also addressed. In addition, we have searched the Simbad database for candidate pulsating binaries. As a result, 322 candidates were extracted. Furthermore, a brief statistics on Algol-type eclipsing binaries (EA) based on the existing catalogs is given. We got 5315 EA, of which there are 904 EA with spectral types A and F. -
Interacting Binaries No
Interacting Binaries No. 16, June 6, 2003 An Electronic Newsletter Editors: Boris T. Gansic¨ ke Dept. of Physics & Astronomy, University of Southampton, Southampton SO17 1BJ, UK Jens Kube Stiftung Alfred-Wegener-Institut fur¨ Polar- und Meeresforschung, Koldewey-Station, N-9173 Ny-Alesund,˚ Norway [email protected], http://astrocat.org/ibnews Contents 1 Editorial 2 2 Abstracts of refereed papers 3 – 1RXS J062518.2+733433: A new intermediate polar Araujo-Betancor et al. 3 – RX J0042.3+4115: a stellar mass black hole binary identified in M31 Barnard et al. 3 – Physical changes during Z-track movement in Sco X-1 on the flaring branch Barnard et al. 4 – Anomalous ultraviolet line flux ratios in the cataclysmic variables 1RXS J232953.9+062814, CE315, BZ UMa and EY Cyg observed with HST/STIS Gansic¨ ke et al. 4 – A new evolutionary channel for Type Ia supernovae King et al. 5 – CVcat: an interactive database on cataclysmic variables Kube et al. 5 – The Fe XXII I(11.92 A)/I(11.77˚ A)˚ Density Diagnostic Applied to the Chandra High Energy Trans- mission Grating Spectrum of EX Hydrae Mauche et al. 5 – The formation of the coronal flow/ADAF Meyer-Hofmeister & Meyer . 6 – The Origin of Soft X-rays in DQ Herculis Mukai et al. 6 – Looking for Dust and Molecules in Nova V4743 Sagittarii Nielbock & Schmidtobreick . 6 – Ultraviolet Spectra of CV Accretion Disks with Non-Steady T(r) Laws Orosz & Wade . 7 – On resonance line profiles predicted by radiation driven disk wind models. Proga . 7 – The emission distribution in RR Pictoris Schmidtobreick et al. -
508-764-2554 Like to Embrace Rather Than Avoid
PROUD MEDIA SPONSOR OF SOUTHBRIDGE AREA RELAY FOR LIFE! SERVING OUR READERS SINCE 1923 WEDNESDAY , M AY 13, 2009 (508) 764-4325/VISIT US AT: www.theheartofmassachusetts.com Newsstand: 60 cents TODAY’S QUOTE A busy June ballot CANDIDATES FOR COUNCIL HEAD LIST “My closest relation 10 BY GUS STEEVES is myself.” NEWS STAFF WRITER SOUTHBRIDGE — For the — Terence last several elections, Southbridge has bucked the tendency of local races to be TOMORROW’S fairly humdrum. This year T ’ is no exception. WEATHER In fact, the June 30 ballot promises to be the most crowded in recent years. Ten people are running for three seats on the Town Council, five for two school committee seats, and two for town clerk. While many names on the list are repeat candidates, there are several new faces. “This is the first [annual election] where pretty much everybody who pulled out papers returned them,” said Showers Town Clerk Madaline High 64 Daoust. “Maybe we’ll get a Low 53 lot more people to come out VFW AWARDS NIGHT to vote.” In fact, just one person, INNING Shawn Kelley photo W INNING who took out papers for Bay all the candidates last night File photo LOTTERY SOUTHBRIDGE — VFW Man of the Year — Southbridge Police Path School Committee, did in an effort to sample the dif- Poll workers go over absentee bal- Chief Daniel Charette — sits with his wife, Kathleen, and son not return them, leaving that ferent views at issue this lots at West Street School to veri- NUMBERS Jacob, 12, at the group’s 63rd annual testimonial banquet seat without a candidate. -
The QANTAS/CROYDON Total Solar Eclipse Flight 23 November 2003 UT
9/23/03 1 The QANTAS/CROYDON Total Solar Eclipse Flight 23 November 2003 UT Mission Planning & Definition Overview REQUIREMENTS for Assisted Real-Time Computation and Navigation Dr. Glenn Schneider, Ph. D. Associate Astronomer & NICMOS Project Instrument Scientist Steward Observatory, The University of Arizona Tucson, Arizona 85750 USA Contact email: [email protected], [email protected] URL: http://nicmosis.as.arizona.edu:8000 Abstract No total solar eclipse has ever been observed from Antarctica both because of the infrequency of occurrence and the logistical complexities associated with Antarctic operations. This paradigm of elusivity regarding Antarctic eclipses in the historical record of science and exploration is about to be broken. The next total solar eclipse, which occurs on 23 November 2003 U.T., the first in the Antarctic since 12 November 1985, will be very largely unobserved due to the geographic remoteness of the path of totality. Yet, interest in securing phenomenological observations of, and associated with, the eclipse by members of the scientific research communities engaged in solar physics, astrodynamics, aeronomy and upper atmospheric physics, as well as educators and amateur astronomers has been extremely high. The development of a flight concept to enable airborne observations, with a dedicated aircraft chartered from QANTAS Airlines, will permit the previously unobtainable to be accomplished. To do so successfully requires detailed preparatory planning for the execution of such a flight. The technical groundwork to achieving this goal has been pursued with diligence over the past four years and is predicated on a legacy and computational infrastructure capability founded on more than three decades of eclipse planning for ground, sea, and airborne venues. -
4.3 Telluric Correction in CARMENES
High precision optical and near-infrared velocimetry with CARMENES Dissertation zur Erlangung des Doktorgrades an der Fakultät für Mathematik, Informatik und Naturwissenschaften Fachbereich Physik der Universität Hamburg vorgelegt von Evangelos Nagel Hamburg 2019 Gutachter der Dissertation: Prof. Dr. Jürgen Schmitt Prof. Dr. Ignasi Ribas Zusammensetzung der Prüfungskommission: Prof. Dr. Jochen Liske Prof. Dr. Jürgen Schmitt Prof. Dr. Robi Banerjee Prof. Dr. Stefan Dreizler Prof. Dr. Dieter Horns Vorsitzende/r der Prüfungskommission: Prof. Dr. Jochen Liske Datum der Disputation: 25.05.2020 Vorsitzender Fach-Promotionsausschusses PHYSIK: Prof. Dr. Günter H. W. Sigl Leiter des Fachbereichs PHYSIK: Prof. Dr. Wolfgang Hansen Dekan der Fakultät MIN: Prof. Dr. Heinrich Graener 2 Abstract The search for Earth-like planets in their habitable zones is one of the main goals in exoplanet research. When orbiting solar-like stars, these planets cause Doppler signals on the order of ∼ 10 cm s−1 over a period of roughly one year. For that reason planet searches started to focus on low-mass stars, where Doppler signals are larger and periods are shorter. A radial velocity based planet search campaign is conducted by CARMENES, which is a spectrometer that operates from the visual to the near-infrared wavelength range. Over a period of several years CARMENES monitors a sample of ∼ 300 M dwarf stars to detect low-mass planets in their habitable zones. In the first part of this thesis I put the focus on how to improve the radial velocity precision of CARMENES by mitigating the effect of the Earth’s atmosphere on the data. Beside stellar mag- netic activity, telluric contamination is one of the main obstacles in achieving higher radial velocity precision. -
Chapter 1. Impact
Atmosphere a Novel Excerpt Chapter 1. Impact our thousand and seventy years ago in a distant part of the Milky Way galaxy, a pair of gravitationally-linked stars began their death spiral, F rumbling into a super energetic state that culminated in a gamma-ray burst beamed at light speed into a then-barren region of the Milky Way. In the 21st Century A.D., the Earth was racing at half a million miles per hour towards a cataclysmic collision with the brief but devastating burst of raw energy from that ancient star explosion. In the city of Papeete, the capital of French Polynesia on the island of Tahiti, children from the local yacht club were on the water with a bevy of single sail dinghies, eight-foot-long training boats with seven-foot sails. Each boat had room for just one child, so the tiny flotilla of snub-nosed boats was being shepherded by two sailing instructors in a motorboat, busily keeping the students corralled within their marked sailing practice area. There was a light breeze, ideal conditions for the Optimus training fleet, with enough force to propel the dinghies wherever the sailors commanded, but not strong enough to flip the boats over. The instructors’ coaching could be clearly heard by the young sailors over the slapping of the waves gently jostling each boat. It was 5:42 in the afternoon of November 23, but the sun was still high. The Milky Way galaxy lay unseen directly overhead the French Polynesian Windward Islands when a blast from a galactic neighbor, a binary star system in the constellation Sagittarius the Archer, descended like Sagittarius’s arrow directly on top of the luckless Tahitians. -
Recurrent Nova IM Normae
A&A 391, L7–L9 (2002) Astronomy DOI: 10.1051/0004-6361:20020985 & c ESO 2002 Astrophysics Recurrent nova IM Normae T. Kato1,H.Yamaoka2, W. Liller3, and B. Monard4 1 Department of Astronomy, Kyoto University, Kyoto 606-8502, Japan 2 Faculty of Science, Kyushu University, Fukuoka 810-8560, Japan 3 Center for Nova Studies, Casilla 5022 Renaca, Vi˜na del Mar, Chile 4 Bronberg Observatory, PO Box 11426, Tiegerpoort 0056, South Africa Letter to the Editor Received 26 March 2002 / Accepted 2 July 2002 Abstract. We detected the second historical outburst of the 1920 nova IM Nor. Accurate astrometry of the outbursting object revealed the true quiescent counterpart having a magnitude of R = 17:0 mag and B = 18:0 mag. We show that the quiescent counterpart shows a noticeable variation. From the comparison of light curves and spectroscopic signatures, we propose that IM Nor and CI Aql comprise a new class of recurrent novae bearing some characteristics similar to those of classical novae. We interpret that the noticeable quiescent variation can be a result of either high orbital inclination, or the presence of high /low states. If the second possibility is confirmed by future observations, IM Nor becomes the first recurrent nova showing state changes in quiescence. Such state changes may provide a missing link between recurrent novae and supersoft X-ray sources. Key words. novae, cataclysmic variables – stars: individual: IM Nor 1. Introduction Table 1. Astrometry of IM Nor. IM Nor was originally discovered as a possible nova in 1920 Source RA Dec Remarks by I. E. -
Tez.Pdf (5.401Mb)
ANKARA ÜNİVERSİTESİ FEN BİLİMLERİ ENSTİTÜSÜ YÜKSEK LİSANS TEZİ ÖRTEN DEĞİŞEN YILDIZLARDA DÖNEM DEĞİŞİMİNİN YILDIZLARIN FİZİKSEL PARAMETRELERİNE BAĞIMLILIĞININ ARAŞTIRILMASI Uğurcan SAĞIR ASTRONOMİ VE UZAY BİLİMLERİ ANABİLİM DALI ANKARA 2006 Her hakkı saklıdır TEŞEKKÜR Tez çalışmam esnasında bana araştırma olanağı sağlayan ve çalışmamın her safhasında yakın ilgi ve önerileri ile beni yönlendiren danışman hocam Sayın Yrd.Doç.Dr. Birol GÜROL’a ve maddi manevi her türlü desteği benden esirgemeyen aileme teşekkürlerimi sunarım. Uğurcan SAĞIR Ankara, Şubat 2006 iii İÇİNDEKİLER ÖZET………………………………………………………………….......................... i ABSTRACT……………………………………………………………....................... ii TEŞEKKÜR……………………………………………………………...................... iii SİMGELER DİZİNİ…………………………………………………….................... vii ŞEKİLLER DİZİNİ...................................................................................................... x ÇİZELGELER DİZİNİ.............................................................................................. xiv 1. GİRİŞ........................................................................................................................ 1 1.1 Çalışmanın Kapsamı................................................................................................ 1 1.2 Örten Çift Sistemlerin Türleri ve Özellikleri........................................................ 1 2. KURAMSAL TEMELLER................................................................................... 3 2.1 Örten Değişen Yıldızlarda Dönem Değişim Nedenleri.................................. -
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 ::::::::::::::::::::::::::::::::::::::::::::::::::: -
Spectroscopic Studies of RV Tau and Related Objects
SPECTROSCOPIC STUDIES OF RV TAU AND RELATED OBJECTS ATHESIS SUBMITTED TO THE MANGALORE UNIVERSITY FOR THE AWARD OF THE DEGREE OF DOCTOR OF PHILOSOPHY IN PHYSICS Submitted by S. SUMANGALA RAO Under the Supervision of PROF.SUNETRA GIRIDHAR INDIAN INSTITUTE OF ASTROPHYSICS BANGALORE - 560 034, INDIA APRIL 2013 To my beloved parents, grand-parents and Niranjan ”I gaze at the sky, To the beauty of stars scattered in many, The clouds do play funny, Hiding firmament in dark, even on days sunny, I, seek nature to reveal elements in stars so earnestly, Am awake whole night with telescopic eye pointing to the sky, Wonder if years rolled by ever slowly? Am I an Astrophysicist to get flash of a spectacular new star? Reflecting in drops of water from a lotus petal forever! Here I’m collecting pearls of wisdom so carefully, Stop not growing with Astrophysics infinitely!”. DECLARATION I hereby declare that the matter contained in the thesis entitled “Spectroscopic Studies of RV Tau and Related Objects” is the result of investigations carried out by me at the Indian Institute of Astrophysics under the supervision of Dr. Sunetra Giridhar. This thesis has not been submitted previously for the award of any degree, diploma, associateship, fellowship etc. of any University or Institute. S. Sumangala Rao (Candidate) Indian Institute of Astrophysics Bangalore-560034, India CERTIFICATE This is to certify that the matter contained in the thesis entitled “Spectroscopic Stud- ies of RV Tau and Related Objects” submitted to Mangalore University by Ms. S. Sumangala Rao for the award of the degree of Doctor of Philosophy in the Faculty of Science, is based on the results of investigations carried out by her under my supervision and guidance, at the Indian Institute of Astrophysics. -
Abstracts (Pdf)
104th Spring Meeting June 4-6, 2015 Muncie, IN ABSTRACTS Friday, June 5, 2015 9:00am – 10:15am Paper Session I Welcome 15 min Horace A. Smith, Mary Anderson, Wayne Osborn, Andrew Layden, Grzegorz Kopacki, Barton Pritzl, Andrew Kelley, Keith McBride, Michael Alexander, Charles Kuehn, Aron Kilian, Eric King, David Carbajal, R. Lustig, Nathan De Lee 20 min “Lightcurves and Period Changes for Type II Cepheids in the Globular Cluster M13” B, V, and Cousins I band lightcurves have been observed for the type II Cepheids V1, V2, and V6 in the globular cluster M13. These are relatively short period, BL Her-type Cepheids, with periods of 1.5, 5.1, and 2.1 days, respectively. Additional observations of V2 have been obtained from early photographic plates in the Yerkes Observatory archive. Long term period changes of these Cepheids have been determined by combining recent photometry with earlier observations that now extend back for more than a century. The observed period changes for V1, V2, and V6 are compared with the predictions of stellar evolution theory, under the assumption that the progenitors of the Cepheids were stars that at one time were on the blue horizontal branch. Dave Cowall 20 min “Multiband CCD Photometry of CY Aquarii using the AAVSOnet” δ Scuti stars are a class of short-period pulsating variable stars that include CY Aquarii. Multiband CCD photometry was performed on that star using AAVSOnet instruments: BSM-HQ, BSM-NM, and BSM-S. Rapid cadence, multi-hour time series yielded high precision light curves and new maxima. Data analyses revealed a pulsation pattern consistent with the existing model that describes the formation of SXPHE stars.