Self-Evaluation Document of the Research Institute of Physics and Astronomy Faculty of Physics and Astronomy Utrecht University
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On the Apparent Absence of Wolf–Rayet+Neutron Star Systems: the Urc Ious Case of WR124 Jesus A
East Tennessee State University Digital Commons @ East Tennessee State University ETSU Faculty Works Faculty Works 12-10-2018 On the Apparent Absence of Wolf–Rayet+Neutron Star Systems: The urC ious Case of WR124 Jesus A. Toala UNAM Campus Morelia Lidi Oskinova University of Potsdam W.R. Hamann University of Potsdam Richard Ignace East Tennessee State University, [email protected] A.A. C. Sander University of Potsdam See next page for additional authors Follow this and additional works at: https://dc.etsu.edu/etsu-works Citation Information Toala, Jesus A.; Oskinova, Lidi; Hamann, W.R.; Ignace, Richard; Sander, A.A. C.; Todt, H.; Chu, Y.H.; Guerrero, M. A.; Hainich, R.; Hainich, R.; and Terrejon, J. M.. 2018. On the Apparent Absence of Wolf–Rayet+Neutron Star Systems: The urC ious Case of WR124. Astrophysical Journal Letters. Vol.869 https://doi.org/10.3847/2041-8213/aaf39d ISSN: 2041-8205 This Article is brought to you for free and open access by the Faculty Works at Digital Commons @ East Tennessee State University. It has been accepted for inclusion in ETSU Faculty Works by an authorized administrator of Digital Commons @ East Tennessee State University. For more information, please contact [email protected]. On the Apparent Absence of Wolf–Rayet+Neutron Star Systems: The Curious Case of WR124 Copyright Statement © 2018. The American Astronomical Society. Reproduced by permission of the AAS. Creator(s) Jesus A. Toala, Lidi Oskinova, W.R. Hamann, Richard Ignace, A.A. C. Sander, H. Todt, Y.H. Chu, M. A. Guerrero, R. Hainich, R. Hainich, and J. M. -
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. -
Star Maps: Where Are the Black Holes?
BLACK HOLE FAQ’s 1. What is a black hole? A black hole is a region of space that has so much mass concentrated in it that there is no way for a nearby object to escape its gravitational pull. There are three kinds of black hole that we have strong evidence for: a. Stellar-mass black holes are the remaining cores of massive stars after they die in a supernova explosion. b. Mid-mass black hole in the centers of dense star clusters Credit : ESA, NASA, and F. Mirabel c. Supermassive black hole are found in the centers of many (and maybe all) galaxies. 2. Can a black hole appear anywhere? No, you need an amount of matter more than 3 times the mass of the Sun before it can collapse to create a black hole. 3. If a star dies, does it always turn into a black hole? No, smaller stars like our Sun end their lives as dense hot stars called white dwarfs. Much more massive stars end their lives in a supernova explosion. The remaining cores of only the most massive stars will form black holes. 4. Will black holes suck up all the matter in the universe? No. A black hole has a very small region around it from which you can't escape, called the “event horizon”. If you (or other matter) cross the horizon, you will be pulled in. But as long as you stay outside of the horizon, you can avoid getting pulled in if you are orbiting fast enough. 5. What happens when a spaceship you are riding in falls into a black hole? Your spaceship, along with you, would be squeezed and stretched until it was torn completely apart as it approached the center of the black hole. -
Astrophysics in 2002
UC Irvine UC Irvine Previously Published Works Title Astrophysics in 2002 Permalink https://escholarship.org/uc/item/8rz4m3tt Journal Publications of the Astronomical Society of the Pacific, 115(807) ISSN 0004-6280 Authors Trimble, V Aschwanden, MJ Publication Date 2003 DOI 10.1086/374651 License https://creativecommons.org/licenses/by/4.0/ 4.0 Peer reviewed eScholarship.org Powered by the California Digital Library University of California Publications of the Astronomical Society of the Pacific, 115:514–591, 2003 May ᭧ 2003. The Astronomical Society of the Pacific. All rights reserved. Printed in U.S.A. Invited Review Astrophysics in 2002 Virginia Trimble Department of Physics and Astronomy, University of California, Irvine, CA 92697; and Astronomy Department, University of Maryland, College Park, MD 20742; [email protected] and Markus J. Aschwanden Lockheed Martin Advanced Technology Center, Solar and Astrophysics Laboratory, Department L9-41, Building 252, 3251 Hanover Street, Palo Alto, CA 94304; [email protected] Received 2003 January 29; accepted 2003 January 29 ABSTRACT. This has been the Year of the Baryon. Some low temperature ones were seen at high redshift, some high temperature ones were seen at low redshift, and some cooling ones were (probably) reheated. Astronomers saw the back of the Sun (which is also made of baryons), a possible solution to the problem of ejection of material by Type II supernovae (in which neutrinos push out baryons), the production of R Coronae Borealis stars (previously-owned baryons), and perhaps found the missing satellite galaxies (whose failing is that they have no baryons). A few questions were left unanswered for next year, and an attempt is made to discuss these as well. -
Grant Proposals, 1991-1999
Grant Proposals, 1991-1999 Finding aid prepared by Smithsonian Institution Archives Smithsonian Institution Archives Washington, D.C. Contact us at [email protected] Table of Contents Collection Overview ........................................................................................................ 1 Administrative Information .............................................................................................. 1 Descriptive Entry.............................................................................................................. 1 Names and Subjects ...................................................................................................... 1 Container Listing ............................................................................................................. 2 Grant Proposals https://siarchives.si.edu/collections/siris_arc_251859 Collection Overview Repository: Smithsonian Institution Archives, Washington, D.C., [email protected] Title: Grant Proposals Identifier: Accession 99-171 Date: 1991-1999 Extent: 17 cu. ft. (17 record storage boxes) Creator:: Smithsonian Astrophysical Observatory. Contracts and Procurement Office Language: English Administrative Information Prefered Citation Smithsonian Institution Archives, Accession 99-171, Smithsonian Astrophysical Observatory, Contracts and Procurement Office, Grant Proposals Descriptive Entry This accession consists of records documenting Smithsonian Astrophysical Observatory projects and activities. Materials include proposals, correspondence, progress -
Neuro-Opthalmology (Developments in Ophthalmology, Vol
Neuro-Ophthalmology Developments in Ophthalmology Vol. 40 Series Editor W. Behrens-Baumann, Magdeburg Neuro- Ophthalmology Neuronal Control of Eye Movements Volume Editors Andreas Straube, Munich Ulrich Büttner, Munich 39 figures, and 3 tables, 2007 Basel · Freiburg · Paris · London · New York · Bangalore · Bangkok · Singapore · Tokyo · Sydney Andreas Straube Ulrich Büttner Department of Neurology Department of Neurology Klinikum Grosshadern Klinikum Grosshadern Marchioninistrasse 15 Marchioninistrasse 15 DE–81377 Munich DE–81377 Munich Library of Congress Cataloging-in-Publication Data Neuro-ophthalmology / volume editors, Andreas Straube, Ulrich Büttner. p. ; cm. – (Developments in ophthalmology, ISSN 0250-3751 ; v. 40) Includes bibliographical references and indexes. ISBN 978-3-8055-8251-3 (hardcover : alk. paper) 1. Neuroophthalmology. I. Straube, Andreas. II. Büttner, U. III. Series. [DNLM: 1. Eye Movements–physiology. 2. Ocular Motility Disorders. 3. Oculomotor Muscles–physiology. 4. Oculomotor Nerve-physiology. W1 DE998NG v.40 2007 / WW 400 N4946 2007] RE725.N45685 2007 617.7Ј32–dc22 2006039568 Bibliographic Indices. This publication is listed in bibliographic services, including Current Contents® and Index Medicus. Disclaimer. The statements, options and data contained in this publication are solely those of the individ- ual authors and contributors and not of the publisher and the editor(s). The appearance of advertisements in the book is not a warranty, endorsement, or approval of the products or services advertised or of their effectiveness, quality or safety. The publisher and the editor(s) disclaim responsibility for any injury to persons or property resulting from any ideas, methods, instructions or products referred to in the content or advertisements. Drug Dosage. The authors and the publisher have exerted every effort to ensure that drug selection and dosage set forth in this text are in accord with current recommendations and practice at the time of publication. -
Evidence for Binary Interaction?!
An Apparent Helical Outflow from a Massive Evolved Star: Evidence for Binary Interaction?! Ryan M. Lau (Caltech/JPL) SOFIA Community Tele-talk Mar 9th, 2016 Collaborators: Matt Hankins, Terry Herter, Mark Morris, Betsy Mills, Mike Ressler An Outline • Background:"Massive"stars"and"the"influence" of"binarity" " • This"Work:"A"dusty,"conical"helix"extending" from"a"Wolf7Rayet"Star" " • The"Future:"Exploring"Massive"Stars"with"the" James"Webb"Space"Telescope" 2" Massive Stars: Galactic Energizers and Refineries • Dominant"sources"of"opFcal"and"UV"photons" heaFng"dust" " • Exhibit"strong"winds,"high"massJloss,"and"dust" producFon"aKer"leaving"the"main"sequence" "" • Explode"as"supernovae"driving"powerful" shocks"and"enriching"the"interstellar"medium" 3" Massive Stars: Galactic Energizers and Refineries Arches"and"Quintuplet"Cluster" at"the"GalacFc"Center" Gal."N" 10"pc" Spitzer/IRAC"(3.6","5.8,"and"8.0"um)" 4" Massive Stars: Galactic Energizers and Refineries Arches"and"Quintuplet"Cluster" at"the"GalacFc"Center" Pistol"Star"and"Nebula" 1"pc" Pa"and"ConFnuum"" 10"pc" Spitzer/IRAC"(3.6","5.8,"and"8.0"um)" 5" Massive stars are not born alone… Binary"InteracCon"Pie"Chart" >70%"of"all"massive" stars"will"exchange" mass"with"companion"" Sana+"(2012)" 6" Influence of Binarity on Stellar Evolution of Massive Stars Binary"InteracCon"Pie"Chart" >70%"of"all"massive" stars"will"exchange" mass"with"companion"" Mass"exchange"will" effect"stellar"luminosity" and"massJloss"rates…" Sana+"(2012)" 7" Influence of Binarity on Stellar Evolution of Massive Stars Binary"InteracCon"Pie"Chart" -
Repetitive Patterns in Rapid Optical Variations in the Nearby Black-Hole Binary V404 Cygni
Repetitive Patterns in Rapid Optical Variations in the Nearby Black-hole Binary V404 Cygni Mariko Kimura1, Keisuke Isogai1, Taichi Kato1, Yoshihiro Ueda1, Satoshi Nakahira2, Megumi Shidatsu3, Teruaki Enoto1,4, Takafumi Hori1, Daisaku Nogami1, Colin Littlefield5, Ryoko Ishioka6, Ying-Tung Chen6, Sun-Kun King6, Chih-Yi Wen6, Shiang-Yu Wang6, Matthew J. Lehner6,7,8, Megan E. Schwamb6, Jen-Hung Wang6, Zhi-Wei Zhang6, Charles Alcock8, Tim Axelrod9, Federica B. Bianco10, Yong-Ik Byun11, Wen-Ping Chen12, Kem H. Cook6, Dae-Won Kim13, Typhoon Lee6, Stuart L. Marshall14, Elena P. Pavlenko15, Oksana I. Antonyuk15, Kirill A. Antonyuk15, Nikolai V. Pit15, Aleksei A. Sosnovskij15, Julia V. Babina15, Aleksei V. Baklanov15, Alexei S. Pozanenko16,17, Elena D. Mazaeva16, Sergei E. Schmalz18, Inna V. Reva19, Sergei P. Belan15, Raguli Ya. Inasaridze20, Namkhai Tungalag21, Alina A. Volnova16, Igor E. Molotov22, Enrique de Miguel23,24, Kiyoshi Kasai25, William Stein26, Pavol A. Dubovsky27, Seiichiro Kiyota28, Ian Miller29, Michael Richmond30, William Goff31, Maksim V. Andreev32,33, Hiromitsu Takahashi34, Naoto Kojiguchi35, Yuki Sugiura35, Nao Takeda35, Eiji Yamada35, Katsura Matsumoto35, Nick James36, Roger D. Pickard37,38, Tamás Tordai39, Yutaka Maeda40, Javier Ruiz41,42,43, Atsushi Miyashita44, Lewis M. Cook45, Akira Imada46 & Makoto Uemura47 1Department of Astronomy, Graduate School of Science, Kyoto University, Oiwakecho, Kitashirakawa, Sakyo-ku, Kyoto 606-8502, Japan! 2JEM Mission Operations and Integration Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan 3MAXI team, RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan 4The Hakubi Center for Advanced Research, Kyoto University, Kyoto 606-8302, Japan 5Astronomy Department, Wesleyan University, Middletown, CT 06459 USA !6Institute of Astronomy and Astrophysics, Academia Sinica, 11F of Astronomy-Mathematics Building, AS/NTU. -
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. -
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. -
The Cataclysmic Variable AE Aquarii: Orbital Variability in V Band
The cataclysmic variable AE Aquarii: orbital variability in V band R. Zamanov & G. Latev Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Tsarigradsko Shose 72, BG-1784 Sofia, Bulgaria [email protected] [email protected] (Submitted on 28.11.2016. Accepted on 31.01.2017) Abstract. We present 62.7 hours observations of the cataclysmic variable AE Aqr in Johnson V band. These are non-published archive electro-photometric data obtained during the time period 1993 to 1999. We construct the orbital variability in V band and obtain a Fourier fit to the double-wave quiescent light curve. The strongest flares in our data set are in phase interval 0.6 - 0.8. The data can be downloaded from http://www.astro.bas.bg/∼rz/DATA/AEAqr.elphot.dat. Key words: Stars: novae, cataclysmic variables – Accretion, accretion disks – white dwarfs – Stars: individual: AE Aqr 1 Introduction AE Aqr is a bright intermediate polar cataclysmic variable (V ≈ 11−12.3). In this semi-detached binary system a spotted K type dwarf (K0-K4 IV/V star) transfers material through the inner Lagrangian point L1 toward a magnetic white dwarf (Skidmore et al. 2003, Hill et al. 2016). It has a relatively long orbital period of 9.88 hours (Robinson et al. 1991; Echevarr´ıa et al. 2008) and an extremely short rotational period of the white dwarf of only 33 s (Patterson et al. 1980). To appear in such a state, AE Aqr should be a former supersoft X-ray binary, in which the mass transfer rate in the recent past (≈ 107 yr) has been much higher than its current value (Schenker et al.