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White dwarf accretion and type Ia supernovae

Proceedings of the International Astronomical Union 2013年第S290期8卷 117-120页

作者： Z. Han X. Chen Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatory Kunming 650011 China email: zhanwenhan@*** cxf@***

Type Ia supernovae (SNe Ia) are believed to be thermonuclear explosions of carbon-oxygen white dwarfs at a mass close to the Chandrasekhar limit. However, a white dwarf at birth has a significantly lower mass and needs to accrete mass to grow to the limit for the explosion. Various progenitor models have been proposed and those models play an important role in our understanding of SNe Ia and cosmology.

关键词： Stars: supernovae stars: white dwarfs

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The 67P/Churyumov-Gerasimenko observation campaign in support of the Rosetta mission

arXiv

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arXiv 2017年

作者： Snodgrass, Colin A’Hearn, M.F. Aceituno, F. Afanasiev, V. Bagnulo, S. Bauer, J. Bergond, G. Besse, S. Biver, N. Bodewits, D. Boehnhardt, H. Bonev, B.P. Borisov, G. Carry, B. Casanova, V. Cochran, A. Conn, B.C. Davidsson, B. Davies, J.K. de León, J. de Mooij, E. de Val-Borro, M. Delacruz, M. DiSanti, M.A. Drew, J.E. Duffard, R. Edberg, N.J.T. Faggi, S. Feaga, L. Fitzsimmons, A. Fujiwara, H. Gibb, E.L. Gillon, M. Green, S.F. Guijarro, A. Guilbert-Lepoutre, A. Gutiérrez, P.J. Hadamcik, E. Hainaut, O. Haque, S. Hedrosa, R. Hines, D. Hopp, U. Hoyo, F. Hutsemékers, D. Hyland, M. Ivanova, O. Jehin, E. Jones, G.H. Keane, J.V. Kelley, M.S.P. Kiselev, N. Kleyna, J. Kluge, M. Knight, M.M. Kokotanekova, R. Koschny, D. Kramer, E. López-Moreno, J.J. Lacerda, P. Lara, L.M. Lasue, J. Lehto, H.J. Levasseur-Regourd, A.C. Licandro, J. Lin, Z.Y. Lister, T. Lowry, S.C. Mainzer, A. Manfroid, J. Marchant, J. McKay, A.J. McNeill, A. Meech, K.J. Micheli, M. Mohammed, I. Monguió, M. Moreno, F. Muñoz, O. Mumma, M.J. Nikolov, P. Opitom, C. Ortiz, J.L. Paganini, L. Pajuelo, M. Pozuelos, F.J. Protopapa, S. Pursimo, T. Rajkumar, B. Ramanjooloo, Y. Ramos, E. Ries, C. Riffeser, A. Rosenbush, V. Rousselot, P. Ryan, E.L. Santos-Sanz, P. Schleicher, D.G. Schmidt, M. Schulz, R. Sen, A.K. Somero, A. Sota, A. Stinson, A. Sunshine, J. Thompson, A. Tozzi, G.P. Tubiana, C. Villanueva, G.L. Wang, X. Wooden, D.H. Yagi, M. Yang, B. Zaprudin, B. Zegmott, T.J. School of Physical Sciences Open University Milton KeynesMK7 6AA United Kingdom Department of Astronomy University of Maryland College ParkMD20742-2421 United States Instituto de Astrofísica de Andalucía CSIC Glorieta de la Astronomía s/n Granada18008 Spain Special Astrophysical Observatory Russian Academy of Sciences Nizhniy Arkhyz Russia Armagh Observatory College Hill ArmaghNorthern IrelandBT61 9DG United Kingdom Jet Propulsion Laboratory M/S 183-301 4800 Oak Grove Drive PasadenaCA91109 United States 04550 Spain ESA/ESAC PO Box 78 Villanueva de la Cañada28691 Spain LESIA Observatoire de Paris CNRS UPMC Univ Paris 06 Univ. Paris-Diderot 5 Place J. Janssen Meudon Pricipal Cedex92195 France Max-Planck-Institut für Sonnensystemforschung Justus-von-Liebig-Weg 3 Göttingen37077 Department of Physics American University 4400 Massachusetts Ave NW WashingtonDC20016 United States Institute of Astronomy and National Astronomical Observatory 72 Tsarigradsko Chaussée Blvd. SofiaBG-1784 Bulgaria Université Côte d’Azur OCA CNRS Lagrange France IMCCE Observatoire de Paris PSL Research University CNRS Sorbonne Universités UPMC Univ Paris 06 Univ. Lille France University of Texas Austin/McDonald Observatory 1 University Station AustinTX78712 United States Research School of Astronomy and Astrophysics Australian National University CanberraACT Australia Gemini Observatory Recinto AURA Colina El Pino s/n Casilla 603 La Serena Chile UK Astronomy Technology Centre Royal Observatory Edinburgh Blackford Hill EdinburghEH9 3HJ C/Vía Láctea s/n La Laguna38205 Spain Departamento de Astrofísica Universidad de La Laguna La Laguna Tenerife38206 Spain Astrophysics Research Centre School of Mathematics and Physics Queen’s University Belfast BT7 1NN United Kingdom Department of Astrophysical Sciences Princeton University PrincetonNJ08544 United States NASA Goddard Space Flight Center Astrochemistry Laboratory Code 691.0 GreenbeltMD20771

We present a summary of the campaign of remote observations that supported the European Space Agency’s Rosetta mission. Telescopes across the globe (and in space) followed comet 67P/Churyumov-Gerasimenko from before Rosetta’s arrival until nearly the end of mission in September 2016. These provided essential data for mission planning, large-scale context information for the coma and tails beyond the spacecraft, and a way to directly compare 67P with other comets. The observations revealed 67P to be a relatively ‘well behaved’ comet, typical of Jupiter family comets and with activity patterns that repeat from orbit-to-orbit. Comparison between this large collection of telescopic observations and the in situ results from Rosetta will allow us to better understand comet coma chemistry and structure. This work is just beginning as the mission ends – in this paper we present a summary of the ground-based observations and early results, and point to many questions that will be addressed in future studies. Copyright © 2017, The Authors. All rights reserved.

关键词： Comets

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Progenitors of type Ia supernovae and their surviving companion stars

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Proceedings of the International Astronomical Union 2013年第S290期8卷 321-322页

作者： B. Wang Z. Liu H. Chen S. Jia Z. Han Yunnan Observatory CAS Kunming 650011 China (email: wangbo@***) Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming 650011 China

Type Ia supernovae (SNe Ia) are the best cosmological distance indicator, however, there is still no agreement on the nature of their progenitors. There are mainly two progenitor scenarios, i.e., the single degenerate (SD) and double degenerate (DD) scenarios. In this article, we introduced our binary evolution models of various progenitor scenarios. We also obtained many properties of the surviving companions from various SD systems, which may be helpful for identifying SN Ia progenitor model. At present, it seems likely that more than one progenitor model may be required to explain the observed diversity of SNe Ia.

关键词： Binaries: close – supernovae: general – white dwarfs

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The refined physical parameters of transiting exoplanet system HAT-P-24

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Research in Astronomy and Astrophysics 2013年第5期13卷 593-603页

作者： Xiao-Bin Wang Sheng-Hong Gu Andrew Collier Cameron Hong-Bo Tan Ho-Keung Hui Chi-Tai Kwok Bill Yeung Kam-Cheung National Astronomical Observatories/Yunnan Observatory Chinese Academy of Sciences Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences School of Physics and Astronomy University of St Andrews North Haugh St Andrews Fife KY16 9SS UK University of Chinese Academy of Sciences Hokoon Nature Education cum Astronomical Centre Sik Sik Yuen Hong Kong Astronomical Society

The transiting exoplanet system HAT-P-24 was observed by using CCD cameras at Yunnan Observatory and Hokoon Astronomical Centre, China in 2010 and 2012. In order to enhance the signal to noise ratio of transit events, the observed data are corrected for systematic errors according to Collier Cameron et al.＇s coarse de- correlation and Tamuz et al.＇s SYSREM algorithms. Three new complete transit light curves are analyzed by means of the Markov chain Monte Carlo technique, and the new physical parameters of the system are derived. They are consistent with the old ones from the discovered paper except for a new larger radius Rp = 1.364 Rj of HAT- P-24b, which confirms its inflated nature. By combining the five available epochs of mid-transit derived from complete transit light curves, the orbital period of HAT-P- 24b is refined to P = 3.3552479 d and no obvious transit timing variation signal can be found from these five transit events during 2010-2012.

关键词： exoplanet system -- transit -- individual： HAT-P-24

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Helium Star Donor Channel to Type Ia Supernovae and Their Surviving Companion Stars

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Proceedings of the International Astronomical Union 2013年第S281期7卷 205-208页

作者： Bo Wang Zhanwen Han National Astronomical Observatories/Yunnan Observatory CAS Kunming 650011 China (email: wangbo@***) Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming 650011 China

Employing Eggleton's stellar evolution code and assuming optically thick winds, we systematically studied the He star donor channel of Type Ia supernovae (SNe Ia), in which a carbon-oxygen white dwarf (WD) accretes material from a He main-sequence star or a He subgiant to increase its mass to the Chandrasekhar mass. We mapped out the initial parameters for producing SNe Ia in the orbital period–secondary mass plane for various WD masses from this channel. Based on a detailed binary population synthesis approach, we find that this channel can produce SNe Ia with short delay times (~100 Myr) implied by recent observations. We derived many properties of the surviving companions of this channel after SN explosion, which can be tested by future observations. We also find that the surviving companions from the SN explosion scenario have a high spatial velocity (>400 km/s), which could be an alternative origin for hypervelocity stars (HVSs), especially for HVSs such as US 708.

关键词： binaries: close — stars: evolution white dwarfs — supernovae: general

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ON GRB PHYSICS REVEALED BY FERMI/LAT

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International Journal of Modern Physics: Conference Series 2013年第23期ijmpcs卷 223-227页

作者： ZHUO LI Department of Astronomy/Kavli Institute for Astronomy and Astrophysics Peking University Beijing 100871 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 China

We discuss the implications of Fermi/LAT observations on several aspects of gamma-ray burst (GRB) physics, including the radiation process, the emission sites, the bulk Lorentz factor, and the pre-shock magnetic field: (1) MeV-range emission favors synchrotron process but the highest energy (> 10 GeV) emission may not be synchrotron origin, more likely inverse Compton origin; (2) GRB should have multi-zone emission region, with MeV emission produced at smaller radii while optical and > 100 MeV emission at larger radii; (3) the bulk Lorentz factor can be a few 100's, much lower than 10 3 , in multi-zone model; (4) the upstream magnetic field of afterglow shock is strongly amplified to be at least in mG scale.

关键词： Gamma-ray burst high energy Fermi/LAT

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ERRATUM: 'GIANT MAGNETAR FLARES IN MULTIPOLAR MAGNETIC FIELDS. I. FULLY AND PARTIALLY OPEN ERUPTIONS OF FLUX ROPES' (2014, ApJ, 784, 168)

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The Astrophysical Journal 2014年第2期787卷

作者： Lei Huang Cong Yu Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai 200030 China Key Laboratory of Radio Astronomy Chinese Academy of Sciences China Key Laboratory for the Structure and Evolution of Celestial Object Chinese Academy of Sciences Kunming 650011 China Yunnan Observatories Chinese Academy of Sciences Kunming 650011 China

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Measurement of the high-energy gamma-ray emission from the Moon with the Fermi Large Area Telescope

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Physical Review D 2016年第8期93卷 082001-082001页

作者： M. Ackermann M. Ajello A. Albert W. B. Atwood L. Baldini G. Barbiellini D. Bastieri R. Bellazzini E. Bissaldi R. D. Blandford R. Bonino E. Bottacini J. Bregeon P. Bruel R. Buehler G. A. Caliandro R. A. Cameron M. Caragiulo P. A. Caraveo E. Cavazzuti C. Cecchi A. Chekhtman J. Chiang G. Chiaro S. Ciprini R. Claus J. Cohen-Tanugi F. Costanza A. Cuoco S. Cutini F. D’Ammando A. de Angelis F. de Palma R. Desiante S. W. Digel L. Di Venere P. S. Drell C. Favuzzi S. J. Fegan W. B. Focke A. Franckowiak S. Funk P. Fusco F. Gargano D. Gasparrini N. Giglietto F. Giordano M. Giroletti T. Glanzman G. Godfrey I. A. Grenier J. E. Grove S. Guiriec A. K. Harding J. W. Hewitt D. Horan X. Hou G. Iafrate G. Jóhannesson T. Kamae M. Kuss S. Larsson L. Latronico J. Li L. Li F. Longo F. Loparco M. N. Lovellette P. Lubrano J. Magill S. Maldera A. Manfreda M. Mayer M. N. Mazziotta P. F. Michelson W. Mitthumsiri T. Mizuno M. E. Monzani A. Morselli S. Murgia E. Nuss N. Omodei E. Orlando J. F. Ormes D. Paneque J. S. Perkins M. Pesce-Rollins V. Petrosian F. Piron G. Pivato S. Rainò R. Rando M. Razzano A. Reimer O. Reimer T. Reposeur C. Sgrò E. J. Siskind F. Spada G. Spandre P. Spinelli H. Takahashi J. B. Thayer D. J. Thompson L. Tibaldo D. F. Torres G. Tosti E. Troja G. Vianello B. L. Winer K. S. Wood M. Yassine F. Cerutti A. Ferrari P. R. Sala Deutsches Elektronen Synchrotron DESY D-15738 Zeuthen Germany Department of Physics and Astronomy Clemson University Kinard Lab of Physics Clemson South Carolina 29634-0978 USA W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics and SLAC National Accelerator Laboratory Stanford University Stanford California 94305 USA Santa Cruz Institute for Particle Physics Department of Physics and Department of Astronomy and Astrophysics University of California at Santa Cruz Santa Cruz California 95064 USA Università di Pisa and Istituto Nazionale di Fisica Nucleare Sezione di Pisa I-56127 Pisa Italy Istituto Nazionale di Fisica Nucleare Sezione di Trieste I-34127 Trieste Italy Dipartimento di Fisica Università di Trieste I-34127 Trieste Italy Istituto Nazionale di Fisica Nucleare Sezione di Padova I-35131 Padova Italy Dipartimento di Fisica e Astronomia “G. Galilei” Università di Padova I-35131 Padova Italy Istituto Nazionale di Fisica Nucleare Sezione di Pisa I-56127 Pisa Italy Istituto Nazionale di Fisica Nucleare Sezione di Bari I-70126 Bari Italy Istituto Nazionale di Fisica Nucleare Sezione di Torino I-10125 Torino Italy Dipartimento di Fisica Generale “Amadeo Avogadro” Università degli Studi di Torino I-10125 Torino Italy Laboratoire Univers et Particules de Montpellier Université Montpellier CNRS/IN2P3 F-34095 Montpellier France Laboratoire Leprince-Ringuet École polytechnique CNRS/IN2P3 F-91128 Palaiseau Cedex France Consorzio Interuniversitario per la Fisica Spaziale (CIFS) I-10133 Torino Italy Dipartimento di Fisica “M. Merlin” dell’Università e del Politecnico di Bari I-70126 Bari Italy INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica I-20133 Milano Italy Agenzia Spaziale Italiana (ASI) Science Data Center I-00133 Roma Italy Istituto Nazionale di Fisica Nucleare Sezione di Perugia I-06123 Perugia Italy Dipartimento di Fisica Università degli Studi di Perugia I-06123 Perugia

We have measured the gamma-ray emission spectrum of the Moon using the data collected by the Large Area Telescope onboard the Fermi satellite during its first seven years of operation, in the energy range from 30 MeV up to a few GeV. We have also studied the time evolution of the flux, finding a correlation with the solar activity. We have developed a full Monte Carlo simulation describing the interactions of cosmic rays with the lunar surface. The results of the present analysis can be explained in the framework of this model, where the production of gamma rays is due to the interactions of cosmic-ray proton and helium nuclei with the surface of the Moon. Finally, we have used our simulation to derive the cosmic-ray proton and helium spectra near Earth from the Moon gamma-ray data.

关键词： Cosmic ray sources Cosmic rays & astroparticles Gamma ray astronomy Solar cycles

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The lifetime of contact binaries

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Proceedings of the International Astronomical Union 2013年第S290期8卷 229-230页

作者： D. K. Jiang Z. W. Han L. H. Yang L. F. Li National Astronomical Observatories Yunnan Observatory Chinese Academy of Sciences P.O. Box 110 Kunming. e-mail: dengkai@*** Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 China

The lifetime of contact binaries is an important parameter for studying the evolution of contact binaries. By reproducing the relative frequency of occurrence for contact binaries, we found that the lifetime of contact binaries decreases with increasing mass of the primaries. The lifetime of contact binaries is about 4%–10% of the main sequence lifetime of the primaries, and is about 0.006–0.65 Gyr. This suggests that the lifetime of contact binaries strongly depends on the mass of the primaries.

关键词： Binaries: close binaries: eclipsing stars: evolution

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The criteria for dynamical mass transfer of the main-sequence donor stars

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Proceedings of the International Astronomical Union 2013年第S290期8卷 213-214页

作者： H. Ge R. F. Webbink X. Chen Z. Han National Astronomical Observatories/Yunnan Observatory Chinese Academy of Sciences Kunming 650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 China Department of Astronomy University of Illinois 1002 W. Green St. Urbana IL 61801 USA

Mass transfer is very common in binary evolution and it dominates the evolutionary fate of binaries. Two crucial problems i.e. dynamical mass transfer and common envelope evolution, are not well understood yet. Here we focus on the first problem, and systematically show the critical mass ratio for dynamical mass transfer when the donor stars are still on the main sequence (MS).

关键词： Binaries:close stars:evolution stars:mass-loss stars:interios

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