DOCSLIB.ORG

Optical Novae As Supersoft X-Ray Sources in the Andromeda Galaxy

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Optical Novae As Supersoft X-Ray Sources in the Andromeda Galaxy T U¨ M¨ M-P-I ¨ P Optical Novae as Supersoft X-ray Sources in the Andromeda Galaxy Martin Henze Vollstandiger¨ Abdruck der von der Fakultat¨ fur¨ Physik der Technischen Universitat¨ Munchen¨ zur Erlangung des akademischen Grades eines Doktors der Naturwissenschaften genehmigten Dissertation. Vorsitzender: Univ.-Prof. Dr. A. Ibarra Prufer¨ der Dissertation: 1. Hon.-Prof. Dr. G. Hasinger 2. Univ.-Prof. Dr. L. Oberauer Die Dissertation wurde am 15.12.2010 bei der Technischen Universitat¨ Munchen¨ eingereicht und durch die Fakultat¨ fur¨ Physik am 17.02.2011 angenommen. T U¨ M¨ Optical Novae as Supersoft X-ray Sources in the Andromeda Galaxy Dissertation von Martin Henze 15. Dezember 2010 M-P-I ¨ P Trick Optical Novae as Supersoft X-ray Sources in the Andromeda Galaxy Optical novae are a subclass of variable stars that display a strong, eruptive increase in their optical luminosity and are sometimes observed as supersoft X-ray sources (SSSs). The physical process responsible for this behaviour is a thermonuclear runaway in an accreted hydrogen envelope on top of a white dwarf in a cataclysmic binary system. This dissertation describes the results from the first dedicated monitoring campaigns for SSS states of optical novae in the central region of the Andromeda galaxy (M 31) with the X-ray telescopes XMM-Newton and Chandra . I present the first analysis of the X-ray properties of the nova population in M 31 based on a statistically significant sample. Peculiar objects from this sample are discussed in detail. Optische Novae als superweiche Rontgenquellen¨ in der Andromedagalaxie Bei optischen Novae handelt es sich um variable Sterne, deren Helligkeit im Optischen wahrend¨ eines singularen¨ Ausbruchs stark zunimmt und die teilweise auch als Rontgenquellen¨ mit extrem weichem Spektrum beobachtet werden. Die physikalische Ursache fur¨ dieses Verhalten ist eine thermonuk- leare Explosion auf der Oberflache¨ eines Weißen Zwergs in einem engen Doppelsternsystem. Meine Dissertation beschreibt Beobachtungen der Andromeda-Galaxie (M 31) mit den Rontgenteleskopen¨ XMM-Newton und Chandra , die erstmals speziell auf die Entdeckung von Novae in Rontgenbereich¨ ausgelegt waren. Das Ziel meiner Arbeit war die erste Untersuchung der Rontgeneigenschaften¨ der Nova-Population in M 31 auf Basis einer statistisch signifikanten Stichprobe. Diese Dissertation stellt die Ergebnisse der Populationsstudie vor und geht naher¨ auf ungewohnliche¨ Einzelquellen ein. Contents 1 Introduction 9 1.1 ClassicalNovae................................... 9 1.1.1 PhysicsofClassicalNovae. ... 9 1.1.2 Optical properties and classification . ......... 9 1.1.3 X-ray properties - classical novae as supersoft X-ray sources ......... 11 1.1.4 Recurrentnovae ................................ 13 1.1.5 NovaeinM31 ................................. 13 1.1.6 Nova population studies . 14 1.1.7 Novae and supersoft X-ray sources in globular star clusters.......... 14 1.1.8 The naming convention for novae in M 31 . ..... 16 1.2 The XMM-Newton, Chandra and Swift X-ray observatories . 16 1.2.1 The XMM-Newton observatory . 17 1.2.2 The Chandra observatory ........................... 18 1.2.3 The Swift observatory ............................. 19 1.3 Dissertation aims and outline . ........ 21 2 Observations and data analysis 23 2.1 Observations .................................... 23 2.1.1 The XMM-Newton/Chandra monitoring of the M 31 central region . 23 2.1.2 Archival X-ray observations of the M 31 central region ............ 25 2.1.3 Optical monitoring of the M 31 central region . ......... 29 2.1.4 Ultraviolet observations of novae with Swift ................. 31 2.2 Dataanalysis .................................... 31 2.2.1 Instrument specific X-ray data processing . ......... 32 2.2.2 General X-ray data analysis procedures . ........ 34 2.2.3 Optical data reduction and analysis . ....... 36 2.2.4 Analysis of Swift ultravioletdata........................ 37 3 Results of the optical and ultraviolet observations 39 3.1 Novae discovered and confirmed in the optical monitoring .............. 39 3.2 Swift ultraviolet detections of novae . 41 4 Results of the X-ray monitoring 43 4.1 Nova counterparts known before this work . .......... 47 4.2 New nova counterparts discovered in this work . ........... 53 4.3 The complete sample of M 31 novae with X-ray counterpart . ............ 68 4.4 Upper limits for non-detected novae . ......... 73 7 4.5 Non-nova supersoft X-ray sources detected in the monitoring............. 80 5 Highlight: First SSSs in M 31 globular clusters 85 5.1 SupersoftsourceinBol111. ..... 85 5.2 SupersoftsourceinBol194. ..... 91 5.2.1 Search for an optical nova counterpart . ........ 92 5.3 Discussion...................................... 96 5.3.1 Globular cluster nova rate - the optical point of view . ............ 96 5.3.2 Globular cluster nova rate - the X-ray point of view . ........... 96 5.3.3 Implications on the nova rate in M 31 globular clusters ............ 97 6 Discussion of the sample of M 31 novae with X-ray counterpart 99 6.1 Short-term variable supersoft X-ray light curves of novae............... 99 6.1.1 M31N2006-04a ................................ 99 6.1.2 M31N2007-12b ................................ 100 6.2 Novae with long supersoft X-ray source states . ............ 100 6.2.1 Two recurrent novae with a very long supersoft X-ray source phase? . 100 6.2.2 Six novae with long supersoft X-ray source states . ........... 101 6.3 Correlations between nova parameters . ......... 102 6.3.1 Supersoft X-ray source turn-on time vs turn-off time ............. 103 6.3.2 Effective blackbody temperature vs X-ray time scales . 104 6.3.3 Optical decay time vs supersoft X-ray source turn-on time .......... 105 6.3.4 Optical expansion velocity vs supersoft X-ray source turn-on time . 105 6.3.5 Physical interpretations - a note of caution . ........... 106 6.4 Derivednovaparameters . 107 6.5 Novae with short supersoft X-ray source states and the completeness of the X-ray monitoring........................................ 109 6.6 Novapopulationstudy ............................. 111 6.7 Asymmetric distribution of novae in X-rays . ........... 113 7 Summary and conclusions 115 A Discoveries of X-ray transients in M 31 i B The curious case of the quasar Sharov 21 vii C Optical light curves from the M 31 centre monitoring xi Acknowledgements xxix Chapter 1 Introduction 1.1 Classical Novae Classical novae (CNe) originate from thermonuclear explosions on the surface of white dwarfs (WDs) in cataclysmic binary systems. This section describes the physics of the nova phenomenon, its op- tical and X-ray properties, and highlights the special role of the Andromeda galaxy (M 31) in nova research. 1.1.1 Physics of Classical Novae The host systems of CNe constitute a subclass of cataclysmic variables (CVs), which are close inter- acting binary star systems (Bode & Evans 2008). The primary component in a CV is a WD. WDs are the final evolutionary stages of stars with initial masses of . 8..10 M⊙ (see e.g. Truran & Livio 1986, and references therein). The secondary component is typically a main-sequence star or a red giant star, which fills its gravitational Roche-lobe (Bode & Evans 2008). This leads to the transfer of matter from the secondary to the WD. If the magnetic field of the WD is not strong, in contrast to AM Her or polar systems, this matter forms an accretion disk around the WD due to conservation of angular momentum. Friction induced energy loss in the accretion disk then causes the matter to settle on the WD’s surface. These processes cause the luminosity of the CV to vary significantly. The variability manifests itself in different observational characteristics for different subtypes of CVs, dependent on the masses and separation of the binary stars and the magnetic field of the WD (see Warner 1995, for an extensive review on CVs). In the case of CNe, the transferred hydrogen-rich matter eventually accumulates on the surface of the WD until hydrogen ignition starts a thermonuclear runaway in the degenerate matter of the WD envelope. The resulting expansion of the hot envelope (see Fig. 1.1) causes the optical brightness of the WD to rise by ∼ 12 magnitudes within a few days, and mass to be ejected at high velocities (see Hernanz 2005; Warner 1995, and references therein). 1.1.2 Optical properties and classification Novae stand out among the plethora of variable star types due to distinctive observational character- istics, although it should be noted that no two novae show exactly the same properties (Bode & Evans 2008). 9 10 Chapter 1. Introduction Figure 1.1: Artist’s impression of a nova occurring on a WD (left) in a close binary system (Credits: Mark A. Garlick, http://www.space-art.co.uk). The light curve of a star describes the evolution of its luminosity over time. Optical light curves of CNe reflect the singular nature of the explosive outburst by showing a rapid rise of the star’s luminosity to the maximum within days. This is followed by a slower decline on time scales of weeks to years back to the pre-outburst luminosity. A schematic nova light curve is shown in Fig. 1.2. Observed nova light curves from the optical monitoring of M 31 are given in Appendix C. Based on the speed of the optical decline, light curves of CNe can be categorised into speed classes, according to the scheme of Payne-Gaposchkin (1964). More precisely, measuring the time the nova luminosity needs to decline by two magnitudes from maximum light, the so-called t2 time, allows the classification the nova as very fast (t2 < 10 days), fast (11 − 25), moderately fast (26 − 80), slow (81 − 150), or very slow (151 − 250) (Bode & Evans 2008). Recently, Strope et al. (2010) introduced a new classification system for nova light curves based on a catalogue of 93 light curves of Galactic novae. This system utilises the shape of the light curve to distinguish seven basic classes, the prototypes of which are shown in Fig.
Load more

Recommended publications
  • Arxiv:2008.06761V1 [Astro-Ph.EP] 15 Aug 2020 We Present a Novel Algorithm to Reduce Scatter and Increase Precision in a Lightcurve Compiled from Many Sources
    , USA Draft version August 18, 2020 Typeset using LATEX modern style in AASTeX62 The visual lightcurve of comet C/1995 O1 (Hale-Bopp) from 1995 - 1999 M. Womack,1, 2 O. Curtis,3 D.A. Rabson,4, 5 O. Harrington Pinto,2 K. Wierzchos,6 S. Cruz Gonzalez,4 G. Sarid,7 C. Mentzer,8 N. Lastra,9 N. Pichette,10 N. Ruffini,11 T. Cox,4 I. Rivera,2 A. Micciche,4 C. Jackson,4 A. Homich,12 A. Tollison,12 S. Reed,12 J. Zilka,12 B. Henning,12 M. Spinar,12 S. Rosslyn Escoto,13 T. Erdahl,12 Marcel P. Goldschen-Ohm,14 and W.T. Uhl15, 16 1Florida Space Institute, University of Central Florida, Orlando FL USA 2Department of Physics, University of Central Florida 3Institute for Astrophysical Research, Boston University, Boston, MA 02215, USA 4Department of Physics, University of South Florida, Tampa, FL 33620, USA 5National Science Foundation, Alexandria, VA 22314, USA 6Catalina Sky Survey, Lunar and Planetary Lab, University of Arizona, Tucson, AZ 85721 7SETI Institute, Mountain View, CA 8Department of Physics and Astronomy, University of Missouri, Columbia, MO 9Department of Physics and Astronomy, Bowling Green State University, OH 10Department of Physics, Montana State University, Bozeman, MT 11Monash University, Australia 12St. Cloud State University, St. Cloud, MN 56301, USA 13Instituto de Astronomia, Universidad Nactional Autonoma de Mexico, Mexico 14Department of Neuroscience, University of Texas at Austin, Austin TX 15Department of Astronomy, Yale University, New Haven, CT 06511 16Dialectic Capital Management, Rowayton, CT 06853 ABSTRACT The long-term brightness evolution of the great comet C/1995 O1 (Hale-Bopp) pre- sented a remarkable opportunity to study the behavior of its coma over four years.
    [Show full text]
  • 1 Accepted for Publication in the Journal of the British
    1 David Elijah Packer: cluster variables, meteors and the solar corona Jeremy Shears Abstract David Elijah Packer (1862-1936), a librarian by profession, was an enthusiastic amateur astronomer who observed from London and Birmingham. He first came to the attention of the astronomical community in 1890 when he discovered a variable star in the globular cluster M5, only the second periodic variable to be discovered in a globular cluster. He also observed meteors and nebulae, on one occasion reporting a brightening in the nucleus of the galaxy M77. However, his remarkable claims in 1896 that he had photographed the solar corona in daylight were soon shown to be flawed. Biographical sketch David Elijah Packer was born in Bermondsey, London, in 1862 April (1) the eldest child of Edward Packer (1820-1896) and Emma (Bidmead) Packer (1831-1918) (2). David attended the Free Grammar School of Saint Olave and Saint John at Southwark, where he performed well, especially in arithmetic, algebra and general mathematics (3). Edward Packer was a basket maker, as was his father and grandfather before him, the Packer family originally coming to London from Thanet, in Kent. The English basket-making industry was in decline during the second half of the nineteenth century due to the availability of cheaper imports from the continent. In spite of this, Edward was still in business in 1881, but the prospects for his son continuing in a trade that had made a living for generations of his ancestors were probably limited (4). Thus at the age of 18 we find David Elijah Packer working as an Oilman’s Assistant, supplying fuel for the oil lamps of London (5).
    [Show full text]
  • Absolute Magnitudes of Asteroids and a Revision of Asteroid Albedo Estimates from WISE Thermal Observations ⇑ Petr Pravec A, , Alan W
    Icarus 221 (2012) 365–387 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations ⇑ Petr Pravec a, , Alan W. Harris b, Peter Kušnirák a, Adrián Galád a,c, Kamil Hornoch a a Astronomical Institute, Academy of Sciences of the Czech Republic, Fricˇova 1, CZ-25165 Ondrˇejov, Czech Republic b 4603 Orange Knoll Avenue, La Cañada, CA 91011, USA c Modra Observatory, Department of Astronomy, Physics of the Earth, and Meteorology, FMFI UK, Bratislava SK-84248, Slovakia article info abstract Article history: We obtained estimates of the Johnson V absolute magnitudes (H) and slope parameters (G) for 583 main- Received 27 February 2012 belt and near-Earth asteroids observed at Ondrˇejov and Table Mountain Observatory from 1978 to 2011. Revised 27 July 2012 Uncertainties of the absolute magnitudes in our sample are <0.21 mag, with a median value of 0.10 mag. Accepted 28 July 2012 We compared the H data with absolute magnitude values given in the MPCORB, Pisa AstDyS and JPL Hori- Available online 13 August 2012 zons orbit catalogs. We found that while the catalog absolute magnitudes for large asteroids are relatively good on average, showing only little biases smaller than 0.1 mag, there is a systematic offset of the cat- Keywords: alog values for smaller asteroids that becomes prominent in a range of H greater than 10 and is partic- Asteroids ularly big above H 12. The mean (H H) value is negative, i.e., the catalog H values are Photometry catalog À Infrared observations systematically too bright.
    [Show full text]
  • AAS NEWSLETTER a Publication for the Members of the American Astronomical Society
    June 2006 Issue 129 AAS NEWSLETTER A Publication for the members of the American Astronomical Society FROM THE (RETIRING) EXECUTIVE OFFICER - BOB MILKEY The past eleven years have been both extremely challenging and rewarding for me in serving as your 3 Executive Officer. Many things have changed over that period and there are still many challenges for Letters to the Society to face. While overall, the Society is in a very good position, I am certainly not passing my the Editor successor a position without ongoing challenges. From my perspective, the most significant AAS accomplishment of the past decade was the introduction 5 of the electronic versions of the AAS journals, but the development of these is still an ongoing process. Chrétien Grant It was well in progress when I joined the Society as the result of an outstanding display of teamwork Award Winner between the AAS staff, volunteers, and the personnel at the University of Chicago Press. At present, the journals are serving the authors and readers well, but both publishing technology and economics are in a state of flux. The challenge will be to introduce new features into the journals while at the same 6 time reducing the overall costs of publication. The choices to be made in balancing these two goals will be best made with input from both the authors and readers of the journals. The stewardship of The Hale & Harvey Astrophysical Journal and The Astronomical Journal is one of the most important services the AAS Prize Winners performs for the astronomical community and arguably the selection of Editors for these journals is one of the most important acts that your elected Council performs.
    [Show full text]
  • X-Ray Monitoring of Optical Novae in M31 from July 2004 to February 2005
    Astronomy & Astrophysics manuscript no. 6812 c ESO 2021 July 7, 2021 X-ray monitoring of optical novae in M 31 from July 2004 to February 2005⋆,⋆⋆ W. Pietsch1, F. Haberl1, G. Sala1, H. Stiele1, K. Hornoch2, A.Riffeser1,3, J. Fliri3, R. Bender1,3, S. B¨uhler3, V. Burwitz1, J. Greiner1, and S. Seitz3 1 Max-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstraße, 85741 Garching, Germany e-mail: [email protected] 2 66431 Lelekovice 393, Czech Republic 3 Universit¨atssternwarte M¨unchen, Scheinerstraße, 81679 M¨unchen, Germany Received 27 November 2006 / Accepted 12 December 2006 ABSTRACT Context. Optical novae have recently been identified as the major class of supersoft X-ray sources in M 31 based on ROSAT and early XMM-Newton and Chandra observations. Aims. This paper reports on a search for X-ray counterparts of optical novae in M 31 based on archival Chandra HRC-I and ACIS-I as well as XMM-Newton observations of the galaxy center region obtained from July 2004 to February 2005. Methods. We systematically determine X-ray brightness or upper limit for counterparts of all known optical novae with outbursts between November 2003 to the end of the X-ray coverage. In addition, we determine the X-ray brightnesses for counterparts of four novae with earlier outbursts. Results. For comparison with the X-ray data we created a catalogue of optical novae in M 31 based on our own nova search programs and on all novae reported in the literature. We collected all known properties and named the novae consistently following the CBAT scheme.
    [Show full text]
  • The Minor Planet Bulletin
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 39, NUMBER 4, A.D. 2012 OCTOBER-DECEMBER 203. 8077 HOYLE: A SHORT PERIOD ASTEROID 2.7454 ± 0.0002 h with an amplitude of 0.20 ± 0.02 mag. While there is a fair amount of scatter in the individual data points, when Daniel A. Klinglesmith III, Ethan Risley, combined they produce a well-determined period, which was Janek Turk, Angelica Vargas found by using an 8th order fit in the FALC analysis algorithm Etscorn Campus Observatory, New Mexico Tech (Harris et al., 1989). 101 East Road Socorro, NM USA 87801 Acknowledgements [email protected] The Etscorn Campus Observatory operations are supported by the Xianming L. Han, Orry R. Heffner, Adam W. Kidd, Research and Economic Development Office of New Mexico Bradley J. Magnetta, Frederick W. Rastede Institute of Mining and Technology (NMIMT). Student support at Department of Physics and Astronomy, Butler University NMIMT is given by NASA EPScOR grant NNX11AQ35A. We Indianapolis, IN USA would like to thank F. Levinson for a generous gift enabling Butler University's membership in the SARA consortium. (Received: 30 May) References The main-belt asteroid 8077 Hoyle was observed on 13 Etscorn Campus Observatory (ECO) (2012). nights over a span of 47 days in 2012 April-May. A http://www.mro.nmt.edu/education-outreach/etscorn-campus- bimodal synodic period of 2.7454 ± 0.0002 h and an observatory/ amplitude of 0.20 ± 0.02 mag. were obtained. Southeastern Association for Research in Astronomy Observatory (SARA) (2012).
    [Show full text]
  • Spin Vector and Shape of (6070) Rheinland and Their Implications
    Spin vector and shape of (6070) Rheinland and their implications David Vokrouhlick´y Institute of Astronomy, Charles University, V Holeˇsoviˇck´ach 2, CZ–18000 Prague 8, Czech Republic, E-mail: [email protected] Josef Durechˇ Institute of Astronomy, Charles University, V Holeˇsoviˇck´ach 2, CZ–18000 Prague 8, Czech Republic David Polishook Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 76100, Israel Yurij N. Krugly Institute of Astronomy, Karazin Kharkiv National University, Sumska 35, Kharkiv 61022, Ukraine Ninel N. Gaftonyuk Crimean Astrophysical Observatory, Simeiz Department, Simeiz 98680, Ukraine Otabek A. Burkhonov arXiv:1111.2061v1 [astro-ph.EP] 8 Nov 2011 Ulugh Beg Astronomical Institute, Uzbek Academy of Sciences, Astronomicheskaya 33, Tashkent 100052, Uzbekistan Shukhrat A. Ehgamberdiev Ulugh Beg Astronomical Institute, Uzbek Academy of Sciences, Astronomicheskaya 33, Tashkent 100052, Uzbekistan Rivkat Karimov –2– Ulugh Beg Astronomical Institute, Uzbek Academy of Sciences, Astronomicheskaya 33, Tashkent 100052, Uzbekistan Igor E. Molotov Keldysh Institute of Applied Mathematics, RAS, Miusskaya sq. 4, Moscow 125047, Russia Petr Pravec Astronomical Institute, Czech Academy of Sciences, Friˇcova 298, CZ–251 65 Ondˇrejov, Czech Republic Kamil Hornoch Astronomical Institute, Czech Academy of Sciences, Friˇcova 298, CZ–251 65 Ondˇrejov, Czech Republic Peter Kuˇsnir´ak Astronomical Institute, Czech Academy of Sciences, Friˇcova 298, CZ–251 65 Ondˇrejov, Czech Republic Julian Oey Leura Observatory, 94 Rawson Pde., Leura, NSW, Australia Adri´an Gal´ad Modra Observatory, Comenius University, Bratislava SK-84248, Slovakia Jindˇrich Ziˇzkaˇ Institute of Astronomy, Charles University, V Holeˇsoviˇck´ach 2, CZ–18000 Prague 8, Czech Republic Received ; accepted Prepared for AJ –3– ABSTRACT Main belt asteroids (6070) Rheinland and (54827) 2001 NQ8 belong to a small population of couples of bodies which reside on very similar heliocentric orbits.
    [Show full text]
  • Správa O Činnosti Organizácie SAV Za Rok 2010
    Astronomický ústav SAV Správa o činnosti organizácie SAV za rok 2010 Tatranská Lomnica január 2011 Obsah osnovy Správy o činnosti organizácie SAV za rok 2010 1. Základné údaje o organizácii 2. Vedecká činnosť 3. Doktorandské ńtúdium, iná pedagogická činnosť a budovanie ľudských zdrojov pre vedu a techniku 4. Medzinárodná vedecká spolupráca 5. Vedná politika 6. Spolupráca s VŃ a inými subjektmi v oblasti vedy a techniky v SR 7. Spolupráca s aplikačnou a hospodárskou sférou 8. Aktivity pre Národnú radu SR, vládu SR, ústredné orgány ńtátnej správy SR a iné organizácie 9. Vedecko-organizačné a popularizačné aktivity 10. Činnosť kniņnično-informačného pracoviska 11. Aktivity v orgánoch SAV 12. Hospodárenie organizácie 13. Nadácie a fondy pri organizácii SAV 14. Iné významné činnosti organizácie SAV 15. Vyznamenania, ocenenia a ceny udelené pracovníkom organizácie SAV 16. Poskytovanie informácií v súlade so zákonom o slobodnom prístupe k informáciám 17. Problémy a podnety pre činnosť SAV PRÍLOHY A Zoznam zamestnancov a doktorandov organizácie k 31.12.2010 B Projekty riešené v organizácii C Publikačná činnosť organizácie D Údaje o pedagogickej činnosti organizácie E Medzinárodná mobilita organizácie Správa o činnosti organizácie SAV 1. Základné údaje o organizácii 1.1. Kontaktné údaje Názov: Astronomický ústav SAV Riaditeľ: RNDr. Aleń Kučera, CSc. Zástupca riaditeľa: doc. RNDr. Ján Svoreņ, DrSc. Vedecký tajomník: RNDr. Drahomír Chochol, DrSc. Predseda vedeckej rady: RNDr. Augustín Skopal, DrSc. Adresa: Astronomický ústav SAV, 059 60 Tatranská Lomnica http://www.ta3.sk Tel.: 052/ 7879 111 Fax: 052/ 4467 656 E-mail: [email protected] Názvy a adresy detašovaných pracovísk: Astronomický ústav - Oddelenie medziplanetárnej hmoty Dúbravská cesta 9, 845 04 Bratislava Vedúci detašovaných pracovísk: Astronomický ústav - Oddelenie medziplanetárnej hmoty Prof.
    [Show full text]
  • Link Between the Potentially Hazardous Asteroid (86039) 1999 NC43 and the Chelyabinsk Meteoroid Tenuous ⇑ Vishnu Reddy A,1, , David Vokrouhlicky´ B, William F
    Icarus 252 (2015) 129–143 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Link between the potentially hazardous Asteroid (86039) 1999 NC43 and the Chelyabinsk meteoroid tenuous ⇑ Vishnu Reddy a,1, , David Vokrouhlicky´ b, William F. Bottke c, Petr Pravec d, Juan A. Sanchez a,1, Bruce L. Gary e, Rachel Klima f, Edward A. Cloutis g, Adrián Galád d, Tan Thiam Guan h, Kamil Hornoch d, Matthew R.M. Izawa g, Peter Kušnirák d, Lucille Le Corre a,1, Paul Mann g, Nicholas Moskovitz i,1, Brian Skiff i, Jan Vraštil b a Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA b Institute of Astronomy, Charles University, V Holešovicˇkách 2, CZ-18000 Prague, Czech Republic c Southwest Research Institute, 1050 Walnut St, Suite 300, Boulder, CO 80302, USA d Astronomical Institute, Academy of Sciences of the Czech Republic, Fricˇova 1, CZ-25165 Ondrˇejov, Czech Republic e Hereford Arizona Observatory, Hereford, AZ 85615, USA f Johns Hopkins University/Applied Physics Laboratory, Laurel, MD, USA g Department of Geography, University of Winnipeg, 515 Portage Avenue, Winnipeg, Manitoba R3B 2E9, Canada h Perth Exoplanet Survey Telescope, 20 Lisle St, Mount Claremont, WA 6010, Australia i Lowell Observatory, 1400 W Mars Hill Road, Flagstaff, AZ 86001, USA article info abstract Article history: We explored the statistical and compositional link between Chelyabinsk meteoroid and potentially haz- Received 31 July 2014 ardous Asteroid (86039) 1999 NC43 to investigate their proposed relation proposed by Borovicˇka et al. Revised 17 December 2014 (Borovicˇka, J., et al. [2013]. Nature 503, 235–237).
    [Show full text]
  • Správa O Činnosti Organizácie
    Publikácie Astronomického ústavu SAV v roku 2010: Vedecké práce v zahraničných karentovaných časopisoch impaktovaných 1. BROŢ, Miroslav - MAYER, Pavel - PRIBULLA, Theodor - ZASCHE, Petr - VOKROUHLICKÝ, David - UHLÁŘ, Robert. A unified solution for the orbit and light-time effect in the V505 Sgr system. In The Astronomical Journal, 2010, vol. 139, p. 2258-2268. (4.481 - IF2009). (2010 - Current Contents, SCOPUS, NASA ADS). ISSN 0004-6256. 2. CARIKOVÁ, Zuzana - SKOPAL, Augustín. Notices to investigation of symbiotic binaries V. Physical parameters derived from UBV magnitudes. In New Astronomy, 2010, vol. 15, p. 637-645. (1.675 - IF2009). (2010 - Current Contents, EBSCO, SCOPUS, NASA ADS). ISSN 1384-1076. 3. DOBROTKA, Andrej - HRIC, Ladislav - CASARES, Jorge - SHAHBAZ, Tariq - MARTÍNEZ-PAIS, Ignacio Gonzales - MUŇOZ-DARIAS, Theodoro. Searching for flickering statistics in T CrB. In Monthly Notices of the Royal Astronomical Society, 2010, vol. 402, p. 2567-2574. (5.103 - IF2009). (2010 - Current Contents, SCOPUS, NASA ADS). ISSN 0035-8711. 4. GAROZZO, Mario - FULVIO, Daniele - KAŇUCHOVÁ, Zuzana - PALUMBO, Maria Elisabetta - STRAZZULLA, Giovanni. The fate of S-bearing species after ion irradiation of interstellar icy grain mantles. In Astronomy and Astrophysics, 2010, vol. 509, article no. A67, p. 1-9. (4.179 - IF2009). (2010 - Current Contents, SCOPUS, NASA ADS). ISSN 0004-6361. 5. GÖMÖRY, Peter - BECK, Christian - BALTHASAR, Horst - RYBÁK, Ján - KUČERA, Aleš - KOZA, Július - WÖHL, Hubertus. Magnetic loop emergence within a granule. In Astronomy and Astrophysics, 2010, vol. 511, article no. 14, p. 1-10. (4.179 - IF2009). (2010 - Current Contents, SCOPUS, NASA ADS). ISSN 0004-6361. 6. HABBAL, S. Rifai - DRUCKMÜLLER, Miloslav - MORGAN, Huw - SCHOLL, Isabelle - RUŠIN, Vojtech - DAW, Adrian - JOHNSON, Judd - ARNDT, Martina.
    [Show full text]
  • Title of the Paper
    Variable Star and Exoplanet Section of Czech Astronomical Society and Masaryk University Proceedings of the 50th Conference on Variable Stars Research Masaryk University (Department of Theoretical Physics and Astrophysics), Brno, Czech Republic 30th November - 2nd December 2018 Editor-in-chief Radek Kocián Participants of the conference OPEN EUROPEAN JOURNAL ON VARIABLE STARS March 2019 http://var.astro.cz/oejv ISSN 1801-5964 TABLE OF CONTENTS The Basic Informatics approach applied to the Modeling and Observations of the QS Virginis System ................ 4 V. BAHYL, M. GAJTANSKA, TINH PHAM VAN Variability of the Spin Periods of Intermediate Polars: Recent Results ................................................................... 8 V. BREUS, I.L. ANDRONOV, P. DUBOVSKY, K. PETRIK, S. ZOLA A new multi-periodic delta Scuti variable in the field of NS Cep .......................................................................... 10 V. DIENSTBIER, M. WOLF & M. SKARKA The peculiar outburst activity of the symbiotic binary AG Draconis ..................................................................... 15 R. GÁLIS, J. MERC, L. LEEDJÄRV, M. VRAŠŤÁK & S. KARPOV Activity of flare star GJ 3236 ................................................................................................................................. 21 J. KÁRA The activity of the symbiotic binary Z Andromedae and its latest outburst .......................................................... 23 J. MERC, R. GÁLIS, M. WOLF, L. LEEDJÄRV, F. TEYSSIER Improvement of Simplified
    [Show full text]
  • 1999 NC43 and the Chelyabinsk Meteoroid Tenuous
    Link between the Potentially Hazardous Asteroid (86039) 1999 NC43 and the Chelyabinsk meteoroid tenuous Vishnu Reddy1 Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA Email: [email protected] David Vokrouhlický Institute of Astronomy, Charles University, V Holešovičkách 2, CZ-18000 Prague, Czech Republic William F. Bottke Southwest Research Institute, 1050 Walnut St, Suite 300, Boulder, CO 80302, USA Petr Pravec Astronomical Institute, Academy of Sciences of the Czech Republic, Fričova 1, CZ- 25165 Ondřejov, Czech Republic Juan A. Sanchez1 Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA Bruce L. Gary Hereford Arizona Observatory, Hereford, AZ, USA Rachel Klima Johns Hopkins University/ Applied Physics Laboratory, Laurel, MD, USA Edward A. Cloutis Department of Geography, University of Winnipeg, 515 Portage Avenue, Winnipeg, Manitoba, Canada R3B 2E9 Adrián Galád Astronomical Institute, Academy of Sciences of the Czech Republic, Fričova 1, CZ- 25165 Ondřejov, Czech Republic Tan Thiam Guan Perth Exoplanet Survey Telescope, 20 Lisle St, Mount Claremont, WA 6010, Australia. Kamil Hornoch Astronomical Institute, Academy of Sciences of the Czech Republic, Fričova 1, CZ- 25165 Ondřejov, Czech Republic Matthew R. M. Izawa 1 Department of Geography, University of Winnipeg, 515 Portage Avenue, Winnipeg, Manitoba, Canada R3B 2E9 Peter Kušnirák Astronomical Institute, Academy of Sciences of the Czech Republic, Fričova 1, CZ- 25165 Ondřejov, Czech Republic Lucille Le Corre1 Planetary Science
    [Show full text]