International Astronomical Union Commission 42 BIBLIOGRAPHY of CLOSE BINARIES No. 93
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Magnificent Spiral Galaxy Is Being Stretched by Passing Neighbor 27 May 2021, by Ray Villard
Magnificent spiral galaxy is being stretched by passing neighbor 27 May 2021, by Ray Villard animals—the gingham dog and calico cat—who got into a spat and ate each other. It's not so dramatic in this case. The galaxies are only getting a little chewed up because of their close proximity. The magnificent spiral galaxy NGC 2276 looks a bit lopsided in this Hubble Space Telescope snapshot. A bright hub of older yellowish stars normally lies directly in the center of most spiral galaxies. But the bulge in NGC 2276 looks offset to the upper left. What's going on? In reality, a neighboring galaxy to the right of NGC 2276 (NGC 2300, not seen here) is gravitationally tugging on its disk of blue stars, pulling the stars on one side of the galaxy outward to distort the galaxy's normal fried-egg appearance. This sort of "tug of war" between galaxies that pass close enough to feel each other's gravitational pull is not uncommon in the universe. But, like Credit: NASA, ESA, STScI, Paul Sell (University of snowflakes, no two close encounters look exactly Florida) alike. In addition, newborn and short-lived massive stars form a bright, blue arm along the upper left edge of The myriad spiral galaxies in our universe almost NGC 2276. They trace out a lane of intense star all look like fried eggs. A central bulge of aging formation. This may have been triggered by a prior stars is like the egg yolk, surrounded by a disk of collision with a dwarf galaxy. -
Opening PANDORA's Box: APEX Observations of CO In
Astronomy & Astrophysics manuscript no. APEX_CO_ArXiv c ESO 2018 November 8, 2018 Opening PANDORA’s box: APEX observations of CO in PNe L. Guzman-Ramirez1; 2, A. I. Gómez-Ruíz3, H. M. J. Boffin4, D. Jones5; 6, R. Wesson7, A. A. Zijlstra8; 9, C. L. Smith10, and Lars-Ake˚ Nyman2; 10 1 Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The Netherlands e-mail: [email protected] 2 European Southern Observatory, Alonso de Córdova 3107, Santiago, Chile 3 CONACYT Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis E. Erro 1, 72840 Tonantzintla, Puebla, México 4 European Southern Observatory, Karl-Schwarzschild-str. 2, D-85748 Garching, Germany 5 Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain 6 Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain 7 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK 8 Jodrell Bank Centre for Astrophysics, University of Manchester, Manchester, UK 9 Department of Physics & Laboratory for Space Research, University of Hong Kong, Pok Fu Lam Road, Hong Kong 10 Centre for Research in Earth and Space Sciences, York University, 4700 Keele Street, Toronto, ON, M3J 1P3, Canada 11 Joint ALMA Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile Received xx, 2018; accepted xx, 2018 ABSTRACT Context. Observations of molecular gas have played a key role in developing the current understanding of the late stages of stellar evolution. Aims. The survey Planetary nebulae AND their cO Reservoir with APEX (PANDORA) was designed to study the circumstellar shells of evolved stars with the aim to estimate their physical parameters. -
HERD Proposal
HERD proposal The Joint Working Team for the HERD collaboration O. Adriani1,2, G. Ambrosi3, Y. Bai4, B. Bertucci3,5, X. Bi6, J. Casaus7, I. De Mitri8,9, M. Dong10, Y. Dong6, I. Donnarumma11, F. Gargano12, E. Liang13, H. Liu13, C. Lyu10, G. Marsella14,15, M.N. Maziotta12, N. Mori2, M. Su16, A. Surdo14, L. Wang4, X. Wu17, Y. Yang10, Q. Yuan18, S. Zhang6, T. Zhang10, L. Zhao10, H. Zhong10, and K. Zhu6 ii 1University of Florence, Department of Physics, I-50019 Sesto Fiorentino, Florence, Italy 2Istituto Nazionale di Fisica Nucleare, Sezione di Firenze, I-50019 Sesto Fiorentino, Florence, Italy 3Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy 4Xi’an Institute of Optics and Precision Mechanics of CAS, 17 Xinxi Road, New Industrial Park, Xi’an Hi-Tech Industrial Development Zone, Xi’an, Shaanxi, China 5Dipartimento di Fisica e Geologia, Universita degli Studi di Perugia, I-06123 Perugia, Italy 6Institute of High Energy Physics, Chinese Academy of Sciences, No. 19B Yuquan Road, Shijingshan District, Beijing 100049, China 7Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas, CIEMAT. Av. Complutense 40, Madrid E-28040, Spain 8Gran Sasso Science Institute (GSSI), Via Iacobucci 2, I-67100, L’Aquila, Italy 9INFN Laboratori Nazionali del Gran Sasso, Assergi, L’Aquila, Italy 10Technology and Engineering Center for Space Utilization, Chinese Academy of Sciences, 9 Dengzhuang South Rd., Haidian Dist., Beijing 100094, China 11Agenzia Spaziale Italiana (ASI), I-00133 Roma, Italy 12Istituto Nazionale di Fisica Nucleare, Sezione di Bari, I-70125, Bari, Italy 13Guangxi University, 100 Daxue East Road, Nanning City, Guangxi, China 14Istituto Nazionale di Fisica Nucleare, Sezione di Lecce, I-73100, Lecce, Italy 15Universita del Salento - Dipartimento di Matematica e Fisica ”E. -
Planetary Nebulae
Planetary Nebulae A planetary nebula is a kind of emission nebula consisting of an expanding, glowing shell of ionized gas ejected from old red giant stars late in their lives. The term "planetary nebula" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years. The mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energizes the shell of nebulous gas around the central star, appearing as a bright colored planetary nebula at several discrete visible wavelengths. Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances. In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. -
Understanding the X-Ray Flaring from N Carinae A
To be Submitted to the Astrophysical Journal Understanding the X-ray Flaring from n Carinae A. F. J. Moffat Departement de physique, UniversiM de Montreal, Succursale Centre-Ville, Montreal, QC, H3C V7, and Centre de recherche en astrophysique du Quebec, Canada [email protected] M. F. Corcoranl CRESST and X-ray Astrophysics Laboratory NASA/GSFC, Greenbelt, jWD 20771, USA [email protected] ABSTRACT We quantify the rapid variations in X-ray brightness ( "flares") from the ex- tremely massive colliding wind binary n Carinae seen during the past three or- bital cycles by RXTE. The observed flares tend to be shorter in duration and more frequent as periastron is approached, although the largest ones tend to be roughly constant in strength at all phases. Plausible scenarios include (1) the largest of multi-scale stochastic wind clumps from the LBV component entering and compressing the hard X-ray emitting wind-wind collision (WWC) zone, (2) large-scale corotating interacting regions in the LBV wind sweeping across the WWC zone, or (3) instabilities intrinsic to the WWC zone. The first one appears to be most consistent with the observations, requiring homologously expanding clumps as they propagate outward in the LBV wind and a turbulence-like power- law distribution of clumps, decreasing in number towards larger sizes, as seen in Wolf-Rayet winds. Subject headings: X-rays: stars — stars: early-type — stars: individual (p Car) — stars: LBV 'Universities Space Research Association, 10211 W incopin Circle. Suite 500 Columbia, 1v1D 21044, USA. -2— 1. Introduction The extremely massive binary star rl Carinae consists of a Luminous Blue Variable (LBV) primary (star A) coupled with a hot, fast-wind secondary (star B) which is probably an evolved 0 star (Verner et al. -
Variable Star Section Circular No
The British Astronomical Association Variable Star Section Circular No. 176 June 2018 Office: Burlington House, Piccadilly, London W1J 0DU Contents Joint BAA-AAVSO meeting 3 From the Director 4 V392 Per (Nova Per 2018) - Gary Poyner & Robin Leadbeater 7 High-Cadence measurements of the symbiotic star V648 Car using a CMOS camera - Steve Fleming, Terry Moon and David Hoxley 9 Analysis of two semi-regular variables in Draco – Shaun Albrighton 13 V720 Cas and its close companions – David Boyd 16 Introduction to AstroImageJ photometry software – Richard Lee 20 Project Melvyn, May 2018 update – Alex Pratt 25 Eclipsing Binary news – Des Loughney 27 Summer Eclipsing Binaries – Christopher Lloyd 29 68u Herculis – David Conner 36 The BAAVSS Eclipsing Binary Programme lists – Christopher Lloyd 39 Section Publications 42 Contributing to the VSSC 42 Section Officers 43 Cover image V392 Per (Nova Per 2018) May 6.129UT iTelescope T11 120s. Martin Mobberley 2 Back to contents Joint BAA/AAVSO Meeting on Variable Stars Warwick University Saturday 7th & Sunday 8th July 2018 Following the last very successful joint meeting between the BAAVSS and the AAVSO at Cambridge in 2008, we are holding another joint meeting at Warwick University in the UK on 7-8 July 2018. This two-day meeting will include talks by Prof Giovanna Tinetti (University College London) Chemical composition of planets in our Galaxy Prof Boris Gaensicke (University of Warwick) Gaia: Transforming Stellar Astronomy Prof Tom Marsh (University of Warwick) AR Scorpii: a remarkable highly variable -
The Hot, Warm and Cold Gas in Arp 227 - an Evolving Poor Group R
The hot, warm and cold gas in Arp 227 - an evolving poor group R. Rampazzo, P. Alexander, C. Carignan, M.S. Clemens, H. Cullen, O. Garrido, M. Marcelin, K. Sheth, G. Trinchieri To cite this version: R. Rampazzo, P. Alexander, C. Carignan, M.S. Clemens, H. Cullen, et al.. The hot, warm and cold gas in Arp 227 - an evolving poor group. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2006, 368, pp.851. 10.1111/j.1365- 2966.2006.10179.x. hal-00083833 HAL Id: hal-00083833 https://hal.archives-ouvertes.fr/hal-00083833 Submitted on 13 Dec 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Mon. Not. R. Astron. Soc. 368, 851–863 (2006) doi:10.1111/j.1365-2966.2006.10179.x The hot, warm and cold gas in Arp 227 – an evolving poor group R. Rampazzo,1 P. Alexander,2 C. Carignan,3 M. S. Clemens,1 H. Cullen,2 O. Garrido,4 M. Marcelin,5 K. Sheth6 and G. Trinchieri7 1Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy 2Astrophysics Group, Cavendish Laboratories, Cambridge CB3 OH3 3Departement´ de physique, Universite´ de Montreal,´ C. -
METEOR CSILLAGÁSZATI ÉVKÖNYV 2019 Meteor Csillagászati Évkönyv 2019
METEOR CSILLAGÁSZATI ÉVKÖNYV 2019 meteor csillagászati évkönyv 2019 Szerkesztette: Benkő József Mizser Attila Magyar Csillagászati Egyesület www.mcse.hu Budapest, 2018 Az évkönyv kalendárium részének összeállításában közreműködött: Tartalom Bagó Balázs Görgei Zoltán Kaposvári Zoltán Kiss Áron Keve Kovács József Bevezető ....................................................................................................... 7 Molnár Péter Sánta Gábor Kalendárium .............................................................................................. 13 Sárneczky Krisztián Szabadi Péter Cikkek Szabó Sándor Szőllősi Attila Zsoldos Endre: 100 éves a Nemzetközi Csillagászati Unió ........................191 Zsoldos Endre Maria Lugaro – Kereszturi Ákos: Elemkeletkezés a csillagokban.............. 203 Szabó Róbert: Az OGLE égboltfelmérés 25 éve ........................................218 A kalendárium csillagtérképei az Ursa Minor szoftverrel készültek. www.ursaminor.hu Beszámolók Mizser Attila: A Magyar Csillagászati Egyesület Szakmailag ellenőrizte: 2017. évi tevékenysége .........................................................................242 Szabados László Kiss László – Szabó Róbert: Az MTA CSFK Csillagászati Intézetének 2017. évi tevékenysége .........................................................................248 Petrovay Kristóf: Az ELTE Csillagászati Tanszékének működése 2017-ben ............................................................................ 262 Szabó M. Gyula: Az ELTE Gothard Asztrofi zikai Obszervatórium -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55 -
Hard X-Ray Emission Clumps in the Γ-Cygni Supernova Remnant: the an INTEGRAL-ISGRI View To
A&A 427, L21–L24 (2004) Astronomy DOI: 10.1051/0004-6361:200400089 & c ESO 2004 Astrophysics Editor Hard X-ray emission clumps in the γ-Cygni supernova remnant: the An INTEGRAL-ISGRI view to A. M. Bykov1, A. M. Krassilchtchikov1 , Yu. A. Uvarov1,H.Bloemen2,R.A.Chevalier3, M. Yu. Gustov1, W. Hermsen2,F.Lebrun4,T.A.Lozinskaya5,G.Rauw6,T.V.Smirnova7, S. J. Sturner8, J.-P. Swings6, R. Terrier4, and I. N. Toptygin1 Letter 1 A. F. Ioffe Institute for Physics and Technology, 26 Polytechnicheskaia, 194021 St. Petersburg, Russia e-mail: [email protected] 2 SRON National Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands 3 Department of Astronomy, University of Virginia, PO Box 3818, Charlottesville, VA 22903, USA 4 CEA – Saclay, DSM/DAPNIA/Service d’Astrophysique, 91191 Gif-sur-Yvette Cedex, France 5 Sternberg Astronomical Institute, Moscow State University, 13 Universitetskij, 119899 Moscow, Russia 6 Institut d’Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août 17, Bât. B5c, 4000 Liège, Belgium 7 Astro Space Center of the Lebedev Physics Institute, 84/32 Profsoyuznaia, 117810 Moscow, Russia 8 NASA Goddard Space Flight Center, Code 661, Greenbelt, MD 20771, USA Received 22 September 2004 / Accepted 9 October 2004 Abstract. Spatially resolved images of the galactic supernova remnant G78.2+2.1 (γ-Cygni) in hard X-ray energy bands from 25 keV to 120 keV are obtained with the IBIS-ISGRI imager aboard the International Gamma-Ray Astrophysics Laboratory INTEGRAL. The images are dominated by localized clumps of about ten arcmin in size. -
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.