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II Publications, Presentations
II Publications, Presentations 1. Refereed Publications Izumi, K., Kotake, K., Nakamura, K., Nishida, E., Obuchi, Y., Ohishi, N., Okada, N., Suzuki, R., Takahashi, R., Torii, Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, Y., Ueda, A., Yamazaki, T.: 2010, DECIGO and DECIGO Search for Gravitational-wave Inspiral Signals Associated with pathfinder, Class. Quantum Grav., 27, 084010. Short Gamma-ray Bursts During LIGO's Fifth and Virgo's First Aoki, K.: 2010, Broad Balmer-Line Absorption in SDSS Science Run, ApJ, 715, 1453-1461. J172341.10+555340.5, PASJ, 62, 1333. Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, All- Aoki, K., Oyabu, S., Dunn, J. P., Arav, N., Edmonds, D., Korista sky search for gravitational-wave bursts in the first joint LIGO- K. T., Matsuhara, H., Toba, Y.: 2011, Outflow in Overlooked GEO-Virgo run, Phys. Rev. D, 81, 102001. Luminous Quasar: Subaru Observations of AKARI J1757+5907, Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, PASJ, 63, S457. Search for gravitational waves from compact binary coalescence Aoki, W., Beers, T. C., Honda, S., Carollo, D.: 2010, Extreme in LIGO and Virgo data from S5 and VSR1, Phys. Rev. D, 82, Enhancements of r-process Elements in the Cool Metal-poor 102001. Main-sequence Star SDSS J2357-0052, ApJ, 723, L201-L206. Abadie, J., et al. including Hayama, K., Kawamura, S.: 2010, Arai, A., et al. including Yamashita, T., Okita, K., Yanagisawa, TOPICAL REVIEW: Predictions for the rates of compact K.: 2010, Optical and Near-Infrared Photometry of Nova V2362 binary coalescences observable by ground-based gravitational- Cyg: Rebrightening Event and Dust Formation, PASJ, 62, wave detectors, Class. -
Harpspol Proposal by C. Neiner
European Organisation for Astronomical Research in the Southern Hemisphere OBSERVING PROGRAMMES OFFICE • Karl-Schwarzschild-Straße 2 • D-85748 Garching bei M¨unchen • e-mail: [email protected] • Tel. : +49 89 320 06473 APPLICATION FOR OBSERVING TIME PERIOD: 95A Important Notice: By submitting this proposal, the PI takes full responsibility for the content of the proposal, in particular with regard to the names of CoIs and the agreement to act according to the ESO policy and regulations, should observing time be granted. 1. Title Category: D{3 Spectropolarimetric observations of BRITE asteroseismic targets: a complete census of magnetic fields in bright stars up to V=4 2. Abstract / Total Time Requested Total Amount of Time: 6 nights VM, 0 hours SM This program aims at observing in circular spectropolarimetry all (yet unobserved) targets of the BRITE constellation of nano-satellites for asteroseismology, i.e. all stars brighter than V=4. They are mainly massive stars and evolved cool stars. Time has already been awarded at CFHT with ESPaDOnS and at TBL with Narval to observe the targets with a declination above -45◦. We propose to observe 104 targets below -45◦ with HarpsPol. Time has already been allocated in P94 for 51 targets. We request here the remaining 53 targets. These data will allow us to (1) obtain a complete and unbiased census of magnetic fields of all stars brighter than V=4, (2) determine the fundamental parameters of all BRITE targets, to constrain the seismic models of BRITE observations; (3) discover new magnetic stars and thus constrain their seismic models even further. -
Winter Constellations
Winter Constellations *Orion *Canis Major *Monoceros *Canis Minor *Gemini *Auriga *Taurus *Eradinus *Lepus *Monoceros *Cancer *Lynx *Ursa Major *Ursa Minor *Draco *Camelopardalis *Cassiopeia *Cepheus *Andromeda *Perseus *Lacerta *Pegasus *Triangulum *Aries *Pisces *Cetus *Leo (rising) *Hydra (rising) *Canes Venatici (rising) Orion--Myth: Orion, the great hunter. In one myth, Orion boasted he would kill all the wild animals on the earth. But, the earth goddess Gaia, who was the protector of all animals, produced a gigantic scorpion, whose body was so heavily encased that Orion was unable to pierce through the armour, and was himself stung to death. His companion Artemis was greatly saddened and arranged for Orion to be immortalised among the stars. Scorpius, the scorpion, was placed on the opposite side of the sky so that Orion would never be hurt by it again. To this day, Orion is never seen in the sky at the same time as Scorpius. DSO’s ● ***M42 “Orion Nebula” (Neb) with Trapezium A stellar nursery where new stars are being born, perhaps a thousand stars. These are immense clouds of interstellar gas and dust collapse inward to form stars, mainly of ionized hydrogen which gives off the red glow so dominant, and also ionized greenish oxygen gas. The youngest stars may be less than 300,000 years old, even as young as 10,000 years old (compared to the Sun, 4.6 billion years old). 1300 ly. 1 ● *M43--(Neb) “De Marin’s Nebula” The star-forming “comma-shaped” region connected to the Orion Nebula. ● *M78--(Neb) Hard to see. A star-forming region connected to the Orion Nebula. -
Title of the Paper
Variable Star and Exoplanet Section of Czech Astronomical Society and Planetarium Ostrava Proceedings of the 51st Conference on Variable Stars Research Planetarium Ostrava, Ostrava, Czech Republic 1st November - 3rd November 2019 Editor-in-chief Radek Kocián Participants of the conference OPEN EUROPEAN JOURNAL ON VARIABLE STARS November 2020 http://oejv.physics.muni.cz ISSN 1801-5964 DOI: 10.5817/OEJV2020-0208 TABLE OF CONTENTS Modeling of GX Lacertae ........................................................................................................................................ 5 Cataclysmic variable CzeV404 Her ......................................................................................................................... 8 On the spin period variability in intermediate polars ............................................................................................. 11 Photometric and spectroscopic observation of symbiotic variables at private observatory Liptovská Štiavnica ... 18 Outburst activity of flare stars 2014 – 2019 ........................................................................................................... 29 2 OPEN EUROPEAN JOURNAL ON VARIABLE STARS November 2020 http://oejv.physics.muni.cz ISSN 1801-5964 DOI: 10.5817/OEJV2020-0208 INTRODUCTION The Variable Star and Exoplanet Section of the Czech Astronomical Society organized traditional autumn conference on research and news in the field of variable stars. The conference was held in a comfortable space of Ostrava Planetarium. In addition -
Správa O Činnosti Organizácie SAV Za Rok 2017
Astronomický ústav SAV Správa o činnosti organizácie SAV za rok 2017 Tatranská Lomnica január 2018 Obsah osnovy Správy o činnosti organizácie SAV za rok 2017 1. Základné údaje o organizácii 2. Vedecká činnosť 3. Doktorandské štúdium, iná pedagogická činnosť a budovanie ľudských zdrojov pre vedu a techniku 4. Medzinárodná vedecká spolupráca 5. Vedná politika 6. Spolupráca s VŠ a inými subjektmi v oblasti vedy a techniky 7. Spolupráca s aplikačnou a hospodárskou sférou 8. Aktivity pre Národnú radu SR, vládu SR, ústredné orgány štátnej správy SR a iné organizácie 9. Vedecko-organizačné a popularizačné aktivity 10. Činnosť knižnično-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 organizácii a 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 31.12.2017 B Projekty riešené v organizácii C Publikačná činnosť organizácie D Údaje o pedagogickej činnosti organizácie E Medzinárodná mobilita organizácie F Vedecko-popularizačná činnosť pracovníkov organizácie SAV Správa o činnosti organizácie SAV 1. Základné údaje o organizácii 1.1. Kontaktné údaje Názov: Astronomický ústav SAV Riaditeľ: Mgr. Martin Vaňko, PhD. Zástupca riaditeľa: Mgr. Peter Gömöry, PhD. Vedecký tajomník: Mgr. Marián Jakubík, PhD. Predseda vedeckej rady: RNDr. Luboš Neslušan, CSc. Člen snemu SAV: Mgr. Marián Jakubík, PhD. Adresa: Astronomický ústav SAV, 059 60 Tatranská Lomnica http://www.ta3.sk Tel.: 052/7879111 Fax: 052/4467656 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. -
Comet C/2018 V1 (Machholz-Fujikawa-Iwamoto): Data Ulate About Past Visits of Interstellar Comets on the Basis of Available Using a 0.47-M Reflector, D
MNRAS 000, 1–11 (2019) Preprint 30 August 2019 Compiled using MNRAS LATEX style file v3.0 Comet C/2018 V1 (Machholz-Fujikawa-Iwamoto): dislodged from the Oort Cloud or coming from interstellar space? C. de la Fuente Marcos1⋆ and R. de la Fuente Marcos2 1 Universidad Complutense de Madrid, Ciudad Universitaria, E-28040 Madrid, Spain 2AEGORA Research Group, Facultad de Ciencias Matemáticas, Universidad Complutense de Madrid, Ciudad Universitaria, E-28040 Madrid, Spain Accepted 2019 August 3. Received 2019 July 26; in original form 2019 February 17 ABSTRACT The chance discovery of the first interstellar minor body, 1I/2017 U1 (‘Oumuamua), indicates that we may have been visited by such objects in the past and that these events may repeat in the future. Unfortunately, minor bodies following nearly parabolic or hyperbolic paths tend to receive little attention: over 3/4 of those known have data-arcs shorter than 30 d and, con- sistently, rather uncertain orbit determinations. This fact suggests that we may have observed interstellar interlopers in the past, but failed to recognize them as such due to insufficient data. Early identification of promising candidates by using N-body simulations may help in improv- ing this situation, triggering follow-up observations before they leave the Solar system. Here, we use this technique to investigate the pre- and post-perihelion dynamical evolution of the slightly hyperbolic comet C/2018 V1 (Machholz-Fujikawa-Iwamoto) to understand its origin and relevance within the context of known parabolic and hyperbolic minor bodies. Based on the available data, our calculations suggest that although C/2018 V1 may be a former mem- ber of the Oort Cloud, an origin beyond the Solar system cannot be excluded. -
Detection of an Increasing Orbital Period in the Subdwarf B Eclipsing System NSVS 14256825 D
CORE Metadata, citation and similar papers at core.ac.uk Provided by University of the Western Cape Research Repository Mon. Not. R. Astron. Soc. 421, 3238–3241 (2012) doi:10.1111/j.1365-2966.2012.20547.x Detection of an increasing orbital period in the subdwarf B eclipsing system NSVS 14256825 D. Kilkenny1 and C. Koen2 1Department of Physics, University of the Western Cape, Private Bag X17, Bellville 7535, South Africa 2Department of Statistics, University of the Western Cape, Private Bag X17, Bellville 7535, South Africa Accepted 2012 January 12. Received 2012 January 12; in original form 2011 December 9 ABSTRACT New timings of eclipses made in 2010 and 2011 are presented for the hot subdwarf B (sdB) eclipsing binary NSVS 14256825. Composed of an sdB star and a much cooler companion, with a period near 0.1104 days, this system is very similar to the prototype sdB eclipsing binary HW Vir. The new observations show that the binary period of NSVS 14256825 is rapidly increasing at a rate of about 12 × 10−12 days orbit−1. Key words: binaries: eclipsing – stars: individual: NSVS 14256825. variables below the period gap might all have arisen from post-sdB 1 INTRODUCTION binary evolution. Close binary stars have long been useful for the determination of In the past few years, it has become clear that continuous orbital fundamental stellar parameters such as mass and radius. Double- period change is not uncommon in HW Vir type systems – very lined spectroscopic binaries enable the mass ratio of the binary close binaries which have hot subdwarf primaries and which show components to be determined, and if the inclination of the binary eclipses, a substantial reflection effect and have typical parame- orbit can be measured or reasonably constrained – as in the case ters R1 ∼ R2 ∼ 0.2R, stellar separations ∼1R and periods of an eclipsing system – then the absolute masses can be found. -
Possible Substellar Companions in Dwarf Eclipsing Binaries: SDSS J143547. 87+ 373338.5, NSVS 7826147, and NSVS 14256825
Astronomy & Astrophysics manuscript no. 39851corr ©ESO 2021 January 22, 2021 Possible substellar companions in dwarf eclipsing binaries: ? SDSS J143547.87+373338.5, NSVS 7826147, and NSVS 14256825 M. Wolf1, H. Kucákovᡠ1; 2; 3, P. Zasche1, K. Hornoch2, J. Kára1, J. Merc1; 4, and M. Zejda5 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University, V Holešovickáchˇ 2, CZ-180 00 Praha 8, Czech Republic, e-mail: [email protected] 2 Astronomical Institute, Academy of Sciences, Fricovaˇ 298, CZ-251 65 Ondrejov,ˇ Czech Republic 3 Research Centre for Theoretical Physics and Astrophysics, Institute of Physics, Silesian University in Opava, Bezrucovoˇ nám. 13, CZ-746 01 Opava, Czech Republic 4 Institute of Physics, Faculty of Science, P. J. Šafárik University, Park Angelinum 9, 040 01 Košice, Slovakia 5 Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlárskᡠ2, CZ-611 37 Brno, Czech Republic Received January 22, 2021 ABSTRACT We present the new results of our long-term observational project to detect the small variations in the orbital periods of low-mass and short-period eclipsing binaries. About 120 new precise mid-eclipse times were obtained for three relatively well-known dwarf eclipsing binaries: SDSS J143547.87+373338.5 (P = 0:126 d), NSVS 07826147 (0.162 d), and NSVS 14256825 (0.110 d). Observed- minus-calculated (O-C) diagrams of these systems were analyzed using all accurate timings, and, where possible, new parameters of the light-time effect were calculated. For the first time, we derive (or improve upon previous findings with regard to) the short orbital periods of 13 and 10 years of possible third bodies for SDSS J143547.87+373338.5 and NSVS 07826147, respectively. -
Dust Near the Sun
Dust Near The Sun Ingrid Mann and Hiroshi Kimura Institut f¨urPlanetologie, Westf¨alischeWilhelms-Universit¨at,M¨unster,Germany Douglas A. Biesecker NOAA, Space Environment Center, Boulder, CO, USA Bruce T. Tsurutani Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA Eberhard Gr¨un∗ Max-Planck-Institut f¨urKernphysik, Heidelberg, Germany Bruce McKibben Department of Physics and Space Science Center, University of New Hampshire, Durham, NH, USA Jer-Chyi Liou Lockheed Martin Space Operations, Houston, TX, USA Robert M. MacQueen Rhodes College, Memphis, TN, USA Tadashi Mukai† Graduate School of Science and Technology, Kobe University, Kobe, Japan Lika Guhathakurta NASA Headquarters, Washington D.C., USA Philippe Lamy Laboratoire d’Astrophysique Marseille, France Abstract. We review the current knowledge and understanding of dust in the inner solar system. The major sources of the dust population in the inner solar system are comets and asteroids, but the relative contributions of these sources are not quantified. The production processes inward from 1 AU are: Poynting- Robertson deceleration of particles outside of 1 AU, fragmentation into dust due to particle-particle collisions, and direct dust production from comets. The loss processes are: dust collisional fragmentation, sublimation, radiation pressure acceler- ation, sputtering, and rotational bursting. These loss processes as well as dust surface processes release dust compounds in the ambient interplanetary medium. Between 1 and 0.1 AU the dust number densities and fluxes can be described by inward extrapolation of 1 AU measurements, assuming radial dependences that describe particles in close to circular orbits. Observations have confirmed the general accuracy of these assumptions for regions within 30◦ latitude of the ecliptic plane. -
HST/STIS Analysis of the First Main Sequence Pulsar CU Virginis
A&A 625, A34 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834937 & © ESO 2019 Astrophysics HST/STIS analysis of the first main sequence pulsar CU Virginis?,?? J. Krtickaˇ 1, Z. Mikulášek1, G. W. Henry2, J. Janík1, O. Kochukhov3, A. Pigulski4, P. Leto5, C. Trigilio5, I. Krtickovᡠ1, T. Lüftinger6, M. Prvák1, and A. Tichý1 1 Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlárskᡠ2, 611 37 Brno, Czech Republic e-mail: [email protected] 2 Center of Excellence in Information Systems, Tennessee State University, Nashville, TN, USA 3 Department of Physics and Astronomy, Uppsala University, Box 516, 751 20 Uppsala, Sweden 4 Astronomical Institute, Wrocław University, Kopernika 11, 51-622 Wrocław, Poland 5 INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy 6 Institut für Astronomie, Universität Wien, Türkenschanzstraße 17, 1180 Wien, Austria Received 20 December 2018 / Accepted 5 March 2019 ABSTRACT Context. CU Vir has been the first main sequence star that showed regular radio pulses that persist for decades, resembling the radio lighthouse of pulsars and interpreted as auroral radio emission similar to that found in planets. The star belongs to a rare group of magnetic chemically peculiar stars with variable rotational period. Aims. We study the ultraviolet (UV) spectrum of CU Vir obtained using STIS spectrograph onboard the Hubble Space Telescope (HST) to search for the source of radio emission and to test the model of the rotational period evolution. Methods. We used our own far-UV and visual photometric observations supplemented with the archival data to improve the parameters of the quasisinusoidal long-term variations of the rotational period. -
Variable Star Classification and Light Curves Manual
Variable Star Classification and Light Curves An AAVSO course for the Carolyn Hurless Online Institute for Continuing Education in Astronomy (CHOICE) This is copyrighted material meant only for official enrollees in this online course. Do not share this document with others. Please do not quote from it without prior permission from the AAVSO. Table of Contents Course Description and Requirements for Completion Chapter One- 1. Introduction . What are variable stars? . The first known variable stars 2. Variable Star Names . Constellation names . Greek letters (Bayer letters) . GCVS naming scheme . Other naming conventions . Naming variable star types 3. The Main Types of variability Extrinsic . Eclipsing . Rotating . Microlensing Intrinsic . Pulsating . Eruptive . Cataclysmic . X-Ray 4. The Variability Tree Chapter Two- 1. Rotating Variables . The Sun . BY Dra stars . RS CVn stars . Rotating ellipsoidal variables 2. Eclipsing Variables . EA . EB . EW . EP . Roche Lobes 1 Chapter Three- 1. Pulsating Variables . Classical Cepheids . Type II Cepheids . RV Tau stars . Delta Sct stars . RR Lyr stars . Miras . Semi-regular stars 2. Eruptive Variables . Young Stellar Objects . T Tau stars . FUOrs . EXOrs . UXOrs . UV Cet stars . Gamma Cas stars . S Dor stars . R CrB stars Chapter Four- 1. Cataclysmic Variables . Dwarf Novae . Novae . Recurrent Novae . Magnetic CVs . Symbiotic Variables . Supernovae 2. Other Variables . Gamma-Ray Bursters . Active Galactic Nuclei 2 Course Description and Requirements for Completion This course is an overview of the types of variable stars most commonly observed by AAVSO observers. We discuss the physical processes behind what makes each type variable and how this is demonstrated in their light curves. Variable star names and nomenclature are placed in a historical context to aid in understanding today’s classification scheme. -
Ice& Stone 2020
Ice & Stone 2020 WEEK 51: DECEMBER 13-19 Presented by The Earthrise Institute # 51 Authored by Alan Hale COMET OF THE WEEK: The Great Comet of 1680 Perihelion: 1680 December 18.49, q = 0.006 AU The Great Comet of 1680 over Rotterdam in The Netherlands, during late December 1680 as painted by the Dutch artist Lieve Verschuier. This particular comet was undoubtedly one of the brightest comets of the 17th Century, but it is also one of the most important comets in history from a scientific perspective, and perhaps even from the perspective of overall human history. While there were certainly plenty of superstitions attached to the comet’s appearance, the scientific investigations made of it were among the beginnings of the era in European history we now call The Enlightenment, and indeed, in a sense the Great Comet of 1680 can perhaps be considered as one of the sparks of that era. The significance began with the comet’s discovery, which was made on the morning of November 14, 1680, by a German astronomer residing in Coburg, Gottfried Kirch – the first comet ever to be discovered by means of a telescope. It was already around 4th magnitude at that time, and located near the star Regulus in the constellation Leo; from that point it traveled eastward and brightened rapidly, being closest to Earth (0.42 AU) on November 30. By that time it was a conspicuous naked-eye object with a tail 20 to 30 degrees long, and it remained visible for another week before disappearing into morning twilight.