Radiation-Driven Stellar Eruptions
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FY08 Technical Papers by GSMTPO Staff
AURA/NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation July 23, 2008 Revised as Complete and Submitted December 23, 2008 NGC 660, ~13 Mpc from the Earth, is a peculiar, polar ring galaxy that resulted from two galaxies colliding. It consists of a nearly edge-on disk and a strongly warped outer disk. Image Credit: T.A. Rector/University of Alaska, Anchorage NATIONAL OPTICAL ASTRONOMY OBSERVATORY NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation December 23, 2008 TABLE OF CONTENTS EXECUTIVE SUMMARY ............................................................................................................................. 1 1 SCIENTIFIC ACTIVITIES AND FINDINGS ..................................................................................... 2 1.1 Cerro Tololo Inter-American Observatory...................................................................................... 2 The Once and Future Supernova η Carinae...................................................................................................... 2 A Stellar Merger and a Missing White Dwarf.................................................................................................. 3 Imaging the COSMOS...................................................................................................................................... 3 The Hubble Constant from a Gravitational Lens.............................................................................................. 4 A New Dwarf Nova in the Period Gap............................................................................................................ -
Asteroseismology with ET
Asteroseismology with ET Erich Gaertig & Kostas D. Kokkotas Theoretical Astrophysics - University of Tübingen nice, et-wp4 meeting,september 1st-2nd, 2010 Asteroseismology with gravitational waves as a tool to probe the inner structure of NS • neutron stars build from single-fluid, normal matter Andersson, Kokkotas (1996, 1998) Benhar, Berti, Ferrari(1999) Benhar, Ferrari, Gualtieri(2004) Asteroseismology with gravitational waves as a tool to probe the inner structure of NS • neutron stars build from single-fluid, normal matter • strange stars composed of deconfined quarks NONRADIAL OSCILLATIONS OF QUARK STARS PHYSICAL REVIEW D 68, 024019 ͑2003͒ NONRADIAL OSCILLATIONS OF QUARK STARS PHYSICAL REVIEW D 68, 024019 ͑2003͒ H. SOTANI AND T. HARADA PHYSICAL REVIEW D 68, 024019 ͑2003͒ FIG. 5. The horizontal axis is the bag constant B (MeV/fmϪ3) Sotani, Harada (2004) FIG. 4. Complex frequencies of the lowest wII mode for each and the vertical axis is the f mode frequency Re(). The squares, stellar model except for the plot for Bϭ471.3 MeV fmϪ3, for circles, and triangles correspond to stellar models whose radiation which the second wII mode is plotted. The labels in this figure radii are fixed at 3.8, 6.0, and 8.2 km, respectively. The dotted line Benhar, Ferrari, Gualtieri, Marassicorrespond (2007) to those of the stellar models in Table I. denotes the new empirical relationship ͑4.3͒ obtained in Sec. IV between Re() of the f mode and B. simple extrapolation to quark stars is not very successful. We want to construct an alternative formula for quark star mod- fixed at Rϱϭ3.8, 6.0, and 8.2 km, and the adopted bag con- els by using our numerical results for f mode QNMs, but we stants are Bϭ42.0 and 75.0 MeV fmϪ3. -
Luminous Blue Variables
Review Luminous Blue Variables Kerstin Weis 1* and Dominik J. Bomans 1,2,3 1 Astronomical Institute, Faculty for Physics and Astronomy, Ruhr University Bochum, 44801 Bochum, Germany 2 Department Plasmas with Complex Interactions, Ruhr University Bochum, 44801 Bochum, Germany 3 Ruhr Astroparticle and Plasma Physics (RAPP) Center, 44801 Bochum, Germany Received: 29 October 2019; Accepted: 18 February 2020; Published: 29 February 2020 Abstract: Luminous Blue Variables are massive evolved stars, here we introduce this outstanding class of objects. Described are the specific characteristics, the evolutionary state and what they are connected to other phases and types of massive stars. Our current knowledge of LBVs is limited by the fact that in comparison to other stellar classes and phases only a few “true” LBVs are known. This results from the lack of a unique, fast and always reliable identification scheme for LBVs. It literally takes time to get a true classification of a LBV. In addition the short duration of the LBV phase makes it even harder to catch and identify a star as LBV. We summarize here what is known so far, give an overview of the LBV population and the list of LBV host galaxies. LBV are clearly an important and still not fully understood phase in the live of (very) massive stars, especially due to the large and time variable mass loss during the LBV phase. We like to emphasize again the problem how to clearly identify LBV and that there are more than just one type of LBVs: The giant eruption LBVs or h Car analogs and the S Dor cycle LBVs. -
Snhunt151: an Explosive Event Inside a Dense Cocoon
MNRAS 475, 2614–2631 (2018) doi:10.1093/mnras/sty009 Advance Access publication 2018 January 9 SNhunt151: an explosive event inside a dense cocoon N. Elias-Rosa,1,2‹ S. Benetti,1 E. Cappellaro,1 A. Pastorello,1 G. Terreran,1 A. Morales-Garoffolo,2 S. C. Howerton,3 S. Valenti,4 E. Kankare,5 A. J. Drake,6 S. G. Djorgovski,6 L. Tomasella,1 L. Tartaglia,1,7 T. Kangas,8 P. Ochner,1 Downloaded from https://academic.oup.com/mnras/article-abstract/475/2/2614/4795309 by Universidad Andres Bello user on 22 April 2019 A. V. Filippenko,9,10 F. Ciabattari,11 S. Geier,12,13 D. A. Howell,14,15 J. Isern,2 S. Leonini,16 G. Pignata17,18 and M. Turatto1 1INAF – Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, I-35122 Padova, Italy 2Department of Applied Physics, University of Cadiz,´ Campus of Puerto Real, E-11510 Cadiz,´ Spain 31401 South A, Arkansas City, KS 67005, USA 4Department of Physics, University of California, Davis, CA 95616, USA 5Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK 6Astronomy Department, California Institute of Technology, Pasadena, CA 91125, USA 7Department of Astronomy and Steward Observatory, University of Arizona, 933 N Cherry Ave, Tucson, AZ 85719, USA 8Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Vais¨ al¨ antie¨ 20, FI-21500 Piikkio,¨ Finland 9Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA 10Miller Senior Fellow, Miller Institute for Basic Research in Science, University of California, -
Communications in Asteroseismology
Communications in Asteroseismology Volume 141 January, 2002 Editor: Michel Breger, TurkÄ enschanzstra¼e 17, A - 1180 Wien, Austria Layout and Production: Wolfgang Zima and Renate Zechner Editorial Board: Gerald Handler, Don Kurtz, Jaymie Matthews, Ennio Poretti http://www.deltascuti.net COVER ILLUSTRATION: Representation of the COROT Satellite, which is primarily devoted to under- standing the physical processes that determine the internal structure of stars, and to building an empirically tested and calibrated theory of stellar evolution. Another scienti¯c goal is to observe extrasolar planets. British Library Cataloguing in Publication data. A Catalogue record for this book is available from the British Library. All rights reserved ISBN 3-7001-3002-3 ISSN 1021-2043 Copyright °c 2002 by Austrian Academy of Sciences Vienna Contents Multiple frequencies of θ2 Tau: Comparison of ground-based and space measurements by M. Breger 4 PMS stars as COROT additional targets by M. Marconi, F. Palla and V. Ripepi 13 The study of pulsating stars from the COROT exoplanet ¯eld data by C. Aerts 20 10 Aql, a new target for COROT by L. Bigot and W. W. Weiss 26 Status of the COROT ground-based photometric activities by R. Garrido, P. Amado, A. Moya, V. Costa, A. Rolland, I. Olivares and M. J. Goupil 42 Mode identi¯cation using the exoplanetary camera by R. Garrido, A. Moya, M. J.Goupil, C. Barban, C. van't Veer-Menneret, F. Kupka and U. Heiter 48 COROT and the late stages of stellar evolution by T. Lebzelter, H. Pikall and F. Kerschbaum 51 Pulsations of Luminous Blue Variables by E. -
Arxiv:1108.0403V1 [Astro-Ph.CO] 1 Aug 2011 Esitps Hleg Oglx Omto Oesadthe and Models Formation Galaxy at to Tion
Noname manuscript No. (will be inserted by the editor) Production of dust by massive stars at high redshift C. Gall · J. Hjorth · A. C. Andersen To be published in A&A Review Abstract The large amounts of dust detected in sub-millimeter galaxies and quasars at high redshift pose a challenge to galaxy formation models and theories of cosmic dust forma- tion. At z > 6 only stars of relatively high mass (> 3 M⊙) are sufficiently short-lived to be potential stellar sources of dust. This review is devoted to identifying and quantifying the most important stellar channels of rapid dust formation. We ascertain the dust production ef- ficiency of stars in the mass range 3–40 M⊙ using both observed and theoretical dust yields of evolved massive stars and supernovae (SNe) and provide analytical expressions for the dust production efficiencies in various scenarios. We also address the strong sensitivity of the total dust productivity to the initial mass function. From simple considerations, we find that, in the early Universe, high-mass (> 3 M⊙) asymptotic giant branch stars can only be −3 dominant dust producers if SNe generate . 3 × 10 M⊙ of dust whereas SNe prevail if they are more efficient. We address the challenges in inferring dust masses and star-formation rates from observations of high-redshift galaxies. We conclude that significant SN dust pro- duction at high redshift is likely required to reproduce current dust mass estimates, possibly coupled with rapid dust grain growth in the interstellar medium. C. Gall Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark Tel.: +45 353 20 519 Fax: +45 353 20 573 E-mail: [email protected] J. -
Urania Nr 5/2001
Eta Carinae To zdjęcie mgławicy otaczającej gwiazdę // Carinae uzyskano za po mocą telskopu kosmicznego Hubble a (K. Davidson i J. Mors). Porównując je z innymi zdjęciami, a w szczególności z obrazem wyko nanym 17 miesięcy wcześniej, Auto rzy stwierdzili rozprężanie się mgła wicy z szybkością ok. 2,5 min km/h, co prowadzi do wniosku, że rozpo częła ona swe istnienie około 150 lat temu. To bardzo ciekawy i intrygujący wynik. Otóż największy znany roz błysk )j Carinae miał miejsce w roku 1840. Wtedy gwiazda ta stała się naj jaśniejszą gwiazdą południowego nie ba i jasność jej przez krótki czas znacznie przewyższała blask gwiaz dy Canopus. Jednak pyłowy dysk ob serwowany wokół)/ Carinae wydaje się być znacznie młodszy - jego wiek (ekspansji) jest oceniany na 100 lat, co może znaczyć, że powstał w cza sie innego, mniejszego wybuchu ob serwowanego w roku 1890. Więcej na temat tego intrygują cego obiektu przeczytać można we wnątrz numeru, w artykule poświę conym tej gwieździe. NGC 6537 Obserwacje przeprowadzone teleskopem Hubble’a pokazały istnienie wielkich falowych struktur w mgławicy Czerwonego Pająka (NGC 6537) w gwiazdozbiorze Strzelca.Ta gorąca i „wietrzna” mgławica powstała wokół jednej z najgorętszych gwiazd Wszech świata, której wiatr gwiazdowy wiejący z prędkością 2000-4500 kilometrów na sekundę wytwarza fale o wysokości 100 miliardów kilometrów. Sama mgławica rozszerza się z szybkością 300 km/s. Jest też ona wyjątkowo gorąca — ok. 10000 K. Sama gwiazda, która utworzyła mgławicę, jest obecnie białym karłem i musi mieć temperaturę nie niższą niż pół miliona stopni — jest tak gorąca, że nie widać jej w obszarach uzyskanych teleskopem Hubble’a, a świeci głównie w promieniowaniu X. -
Stats2010 E Final.Pdf
Imprint Publisher: Max-Planck-Institut für extraterrestrische Physik Editors and Layout: W. Collmar und J. Zanker-Smith Personnel 1 PERSONNEL 2010 Directors Min. Dir. J. Meyer, Section Head, Federal Ministry of Prof. Dr. R. Bender, Optical and Interpretative Astronomy, Economics and Technology also Professorship for Astronomy/Astrophysics at the Prof. Dr. E. Rohkamm, Thyssen Krupp AG, Düsseldorf Ludwig-Maximilians-University Munich Prof. Dr. R. Genzel, Infrared- and Submillimeter- Scientifi c Advisory Board Astronomy, also Prof. of Physics, University of California, Prof. Dr. R. Davies, Oxford University (UK) Berkeley (USA) (Managing Director) Prof. Dr. R. Ellis, CALTECH (USA) Prof. Dr. Kirpal Nandra, High-Energy Astrophysics Dr. N. Gehrels, NASA/GSFC (USA) Prof. Dr. G. Morfi ll, Theory, Non-linear Dynamics, Complex Prof. Dr. F. Harrison, CALTECH (USA) Plasmas Prof. Dr. O. Havnes, University of Tromsø (Norway) Prof. Dr. G. Haerendel (emeritus) Prof. Dr. P. Léna, Université Paris VII (France) Prof. Dr. R. Lüst (emeritus) Prof. Dr. R. McCray, University of Colorado (USA), Prof. Dr. K. Pinkau (emeritus) Chair of Board Prof. Dr. J. Trümper (emeritus) Prof. Dr. M. Salvati, Osservatorio Astrofi sico di Arcetri (Italy) Junior Research Groups and Minerva Fellows Dr. N.M. Förster Schreiber Humboldt Awardee Dr. S. Khochfar Prof. Dr. P. Henry, University of Hawaii (USA) Prof. Dr. H. Netzer, Tel Aviv University (Israel) MPG Fellow Prof. Dr. V. Tsytovich, Russian Academy of Sciences, Prof. Dr. A. Burkert (LMU) Moscow (Russia) Manager’s Assistant Prof. S. Veilleux, University of Maryland (USA) Dr. H. Scheingraber A. v. Humboldt Fellows Scientifi c Secretary Prof. Dr. D. Jaffe, University of Texas (USA) Dr. -
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 ::::::::::::::::::::::::::::::::::::::: -
Asteroseismic Fingerprints of Stellar Mergers
MNRAS 000,1–13 (2021) Preprint 7 September 2021 Compiled using MNRAS LATEX style file v3.0 Asteroseismic Fingerprints of Stellar Mergers Nicholas Z. Rui,1¢ Jim Fuller1 1TAPIR, California Institute of Technology, Pasadena, CA 91125, USA Accepted XXX. Received YYY; in original form ZZZ ABSTRACT Stellar mergers are important processes in stellar evolution, dynamics, and transient science. However, it is difficult to identify merger remnant stars because they cannot easily be distinguished from single stars based on their surface properties. We demonstrate that merger remnants can potentially be identified through asteroseismology of red giant stars using measurements of the gravity mode period spacing together with the asteroseismic mass. For mergers that occur after the formation of a degenerate core, remnant stars have over-massive envelopes relative to their cores, which is manifested asteroseismically by a g mode period spacing smaller than expected for the star’s mass. Remnants of mergers which occur when the primary is still on the main sequence or whose total mass is less than ≈2 " are much harder to distinguish from single stars. Using the red giant asteroseismic catalogs of Vrard et al.(2016) and Yu et al.(2018), we identify 24 promising candidates for merger remnant stars. In some cases, merger remnants could also be detectable using only their temperature, luminosity, and asteroseismic mass, a technique that could be applied to a larger population of red giants without a reliable period spacing measurement. Key words: asteroseismology—stars: evolution—stars: interiors—stars: oscillations 1 INTRODUCTION for the determination of evolutionary states (Bedding et al. 2011; Bildsten et al. -
A Blast Wave from the 1843 Eruption of Eta Carinae
1 A Blast Wave from the 1843 Eruption of Eta Carinae Nathan Smith* *Astronomy Department, University of California, 601 Campbell Hall, Berkeley, CA 94720-3411 Very massive stars shed much of their mass in violent precursor eruptions [1] as luminous blue variables (LBVs) [2] before reaching their most likely end as supernovae, but the cause of LBV eruptions is unknown. The 19th century eruption of Eta Carinae, the prototype of these events [3], ejected about 12 solar masses at speeds of 650 km/s, with a kinetic energy of almost 1050ergs[4]. Some faster material with speeds up to 1000-2000 km/s had previously been reported [5,6,7,8] but its full distribution was unknown. Here I report observations of much faster material with speeds up to 3500-6000 km/s, reaching farther from the star than the fastest material in earlier reports [5]. This fast material roughly doubles the kinetic energy of the 19th century event, and suggests that it released a blast wave now propagating ahead of the massive ejecta. Thus, Eta Carinae’s outer shell now mimics a low-energy supernova remnant. The eruption has usually been discussed in terms of an extreme wind driven by the star’s luminosity [2,3,9,10], but fast material reported here suggests that it was powered by a deep-seated explosion rivalling a supernova, perhaps triggered by the pulsational pair instability[11]. This may alter interpretations of similar events seen in other galaxies. Eta Carinae [3] is the most luminous and the best studied among LBVs [1,2]. -
NASA's Goddard Space Flight Center Laboratory for Astronomy & Solar Physics Greenbelt, Maryland, 20771
NASA’s Goddard Space Flight Center Laboratory for Astronomy & Solar Physics Greenbelt, Maryland, 20771 The following report covers the period from Septem- istrator announced the cancellation of the next servicing ber 2003 through September 2004. mission (SM4) to the Hubble Space Telescope (HST), citing safety concerns about sending the Shuttle into an 1 INTRODUCTION orbit that did not have a “safe haven” (namely, the Inter- The Laboratory for Astronomy & Solar Physics national Space Station). Subsequently, the Administra- (LASP) is a Division of the Space Sciences Directorate tor authorized GSFC to begin study of a robotic repair at NASA’s Goddard Space Flight Center (GSFC). Mem- of HST, which would add new batteries, gyroscopes, and bers of LASP conduct a broad program of observational install both of the new instruments intended for installa- and theoretical scientific research. Observations are car- tion on SM4 – the Cosmic Origins Spectrograph (COS) ried out from space-based observatories, balloons, and and the Wide Field Camera 3 (WFC3). An intensive ground-based telescopes at wavelengths extending from engineering effort in the HST Project at Goddard is cur- the EUV to the sub-millimeter. Research projects cover rently underway to determine if this robotic repair is the fields of solar and stellar astrophysics, extrasolar technically possible within the allowed time-fame (be- planets, the interstellar and intergalactic medium, ac- fore the HST batteries die). WFC3 has completed a tive galactic nuclei, and the evolution of structure in the successful initial thermal vacuum test at Goddard under universe. the leadership of Instrument Scientist Randy Kimble. Studies of the sun are carried out in the gamma- However, on a decidedly sad note for LASP, the Space ray, x-ray, EUV/UV and visible portions of the spec- Telescope Imaging Spectrograph (STIS; Woodgate, PI), trum from space and the ground.