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High velocity and hypervelocity stars from the companions of type Ia supernovae

Proceedings of the International Astronomical Union 2014年第S298期9卷 443-443页

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

The single-degenerate (SD) model is currently a favourable progenitor scenario for the production of type Ia supernovae (SNe Ia). The companion in the SD model would survive after the SN explosion. In this work, we obtained the velocity distribution of the surviving companion stars from different SD scenarios in the Galaxy, which can be verified by future observations.

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

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Velocity distributions of surviving companion stars of type Ia supernovae in the Milky Way

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Proceedings of the International Astronomical Union 2014年第S298期9卷 413-413页

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

The companion stars of type Ia supernovae (SNe Ia) would survive the explosions and show peculiar properties in the single-degenerate (SD) scenario. Whit different SD SN Ia channels, we obtained the velocity distributions of the surviving companion stars in the Milky Way. All properties presented may be verified by future observations.

关键词： binaries: close – supernovae: general – Galaxy: kinematics and dynamics

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OBSERVATIONS OF M31 AND M33 WITH THE FERMI LARGE AREA TELESCOPE: A GALACTIC CENTER EXCESS IN ANDROMEDA?

arXiv

引用

arXiv 2017年

作者： Ackermann, M. Ajello, M. Albert, A. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bellazzini, R. Bissaldi, E. Bloom, E.D. Bonino, R. Bottacini, E. Brandt, T.J. Bregeon, J. Bruel, P. Buehler, R. Cameron, R.A. Caputo, R. Caragiulo, M. Caraveo, P.A. Cavazzuti, E. Cecchi, C. Charles, E. Chekhtman, A. Chiaro, G. Ciprini, S. Costanza, F. Cutini, S. D’Ammando, F. de Palma, F. Desiante, R. Digel, S.W. Di Lalla, N. Di Mauro, M. Di Venere, L. Favuzzi, C. Funk, S. Fusco, P. Gargano, F. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Green, D. Grenier, I.A. Guillemot, L. Guiriec, S. Hayashi, K. Hou, X. Jóhannesson, G. Kamae, T. Knödlseder, J. Kong, A.K.H. Kuss, M. la Mura, G. Larsson, S. Latronico, L. Li, J. Longo, F. Loparco, F. Lubrano, P. Maldera, S. Malyshev, D. Manfreda, A. Martin, P. Mazziotta, M.N. Michelson, P.F. Mirabal, N. Mitthumsiri, W. Mizuno, T. Monzani, M.E. Morselli, A. Moskalenko, I.V. Negro, M. Nuss, E. Ohsugi, T. Omodei, N. Orlando, E. Ormes, J.F. Paneque, D. Persic, M. Pesce-Rollins, M. Piron, F. Porter, T.A. Principe, G. Rainò, S. Rando, R. Razzano, M. Reimer, O. Sánchez-Conde, M. Sgrò, C. Simone, D. Siskind, E.J. Spada, F. Spandre, G. Spinelli, P. Tanaka, K. Tibaldo, L. Torres, D.F. Troja, E. Uchiyama, Y. Wang, J.C. Wood, K.S. Wood, M. Zaharijas, G. Zhou, M. Deutsches Elektronen Synchrotron DESY ZeuthenD-15738 Germany Department of Physics and Astronomy Clemson University Kinard Lab of Physics ClemsonSC29634-0978 United States Los Alamos National Laboratory Los AlamosNM87545 United States Università di Pisa Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Laboratoire AIM CEA-IRFU CNRS Université Paris Diderot Service d’Astrophysique CEA Saclay Gif sur YvetteF-91191 France Istituto Nazionale di Fisica Nucleare Sezione di Trieste TriesteI-34127 Italy Dipartimento di Fisica Università di Trieste TriesteI-34127 Italy Istituto Nazionale di Fisica Nucleare Sezione di Padova PadovaI-35131 Italy Dipartimento di Fisica e Astronomia "G. Galilei" Università di Padova PadovaI-35131 Italy Istituto Nazionale di Fisica Nucleare Sezione di Pisa PisaI-56127 Italy Istituto Nazionale di Fisica Nucleare Sezione di Bari BariI-70126 Italy W. W. Hansen Experimental Physics Laboratory Kavli Institute for Particle Astrophysics and Cosmology Department of Physics SLAC National Accelerator Laboratory Stanford University StanfordCA94305 United States Istituto Nazionale di Fisica Nucleare Sezione di Torino TorinoI-10125 Italy Dipartimento di Fisica Università degli Studi di Torino TorinoI-10125 Italy NASA Goddard Space Flight Center GreenbeltMD20771 United States Laboratoire Univers et Particules de Montpellier Université Montpellier CNRS/IN2P3 MontpellierF-34095 France Laboratoire Leprince-Ringuet École polytechnique CNRS/IN2P3 PalaiseauF-91128 France Santa Cruz Institute for Particle Physics Department of Physics Department of Astronomy and Astrophysics University of California at Santa Cruz Santa CruzCA95064 United States Dipartimento di Fisica "M. Merlin" dell’Università e del Politecnico di Bari BariI-70126 Italy INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Milano via E. Bassini 15 MilanoI-20133 Italy Science Data Center RomaI-00133 Italy Istituto Nazionale di Fi

The Fermi Large Area Telescope (LAT) has opened the way for comparative studies of cosmic rays (CRs) and high-energy objects in the Milky Way (MW) and in other, external, star-forming galaxies. Using 2 yr of observations with the Fermi LAT, Local Group galaxy M31 was detected as a marginally extended gamma-ray source, while only an upper limit has been derived for the other nearby galaxy M33. We revisited the gamma-ray emission in the direction of M31 and M33 using more than 7 yr of LAT Pass 8 data in the energy range 0.1−100 GeV, presenting detailed morphological and spectral analyses. M33 remains undetected, and we computed an upper limit of 2.0×10−12 erg cm−2 s−1 on the 0.1−100 GeV energy flux (95% confidence level). This revised upper limit remains consistent with the observed correlation between gamma-ray luminosity and star-formation rate tracers and implies an average CR density in M33 that is at most half of that of the MW. M31 is detected with a significance of nearly 10σ. Its spectrum is consistent with a power law with photon index Γ = 2.4±0.1stat+syst and a 0.1−100 GeV energy flux of (5.6±0.6stat+syst)×10−12 erg cm−2 s−1. M31 is detected to be extended with a 4σ significance. The spatial distribution of the emission is consistent with a uniform-brightness disk with a radius of 0◦.4 and no offset from the center of the galaxy, but nonuniform intensity distributions cannot be excluded. The flux from M31 appears confined to the inner regions of the galaxy and does not fill the disk of the galaxy or extend far from it. The gamma-ray signal is not correlated with regions rich in gas or star-formation activity, which suggests that the emission is not interstellar in origin, unless the energetic particles radiating in gamma rays do not originate in recent star formation. Alternative and nonexclusive interpretations are that the emission results from a population of millisecond pulsars dispersed in the bulge and disk of M31 by disrupted globular clusters or from

关键词： Galaxies

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Interactions between planets and evolved stars

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Journal of Physics: Conference Series 2016年第4期728卷

作者： Qian Shengbang Han Zhongtao E Fernández Lajús Zhu liying Liao Wenping Zejda Miloslav Li Linjia Irina Voloshina Liu Liang He Jiajia. Yunnan Observatories Chinese Academy of Sciences P.O. Box 110 650216 Kunming P.R. China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P.O. Box 110 650216 Kunming P. R. China University of the Chinese Academy of Sciences Yuquan Road 19# Shijingshan Block 100049 Beijing P. R. China Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata 1900 La Plata Buenos Aires Argentina Instituto de Astrofisica de La Plata (CCT La plata - CONICET/UNLP) Argentina Visiting Astronomer Complejo Astronómico El Leoncito operated under agreement between the Consejo Nacional de Investigaciones Científicas y Técnicas de la República Argentina and the National Universities of La Plata Córdoba and San Juan. Department of Theoretical Physics and Astrophysics Masaryk University Kotlářská 2 CZ-611 37 Brno Czech Republic Sternberg Astronomical Institute Moscow State University Universitetskij prospect 13 Moscow 119992 Russia

Searching for planetary companions to evolved stars (e.g., white dwarfs (WD) and Cataclysmic Variables (CV)) can provide insight into the interaction between planets and evolved stars as well as on the ultimate fate of planets. We have monitored decades of CVs and their progenitors including some detached WD binaries since 2006 to search for planets orbiting these systems. In the present paper, we will show some observational results of circumbinary planets in orbits around CVs and their progenitors. Some of our findings include planets with the shortest distance to the central evolved binaries and a few multiple planetary systems orbiting binary stars. Finally, by comparing the observational properties of planetary companions to single WDs and WD binaries, the interaction between planets and evolved stars and the ultimate fate of planets are discussed.

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A binary evolution model with non-synchronous rotations

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Chinese Astronomy and Astrophysics 2013年第1期37卷 41-59页

作者： Rui-yu, Zhang Yan, Li Yunnan Astronomical Observatory Chinese Academy of Sciences Kunming 650011 China Graduate University of Chinese Academy of Sciences Beijing 100049 China Key Laboratory of the Structure and Evolution of celestial Objects Chinese Academy of Sciences Kunming 650011 China

By calculating the angular momentum transport during the evolution of a binary system, the variations of the rotational and revolution periods of the binary system under the tidal action, as well as the tidal effect on the evolution of the system are investigated. The calculated results indicate that when a close binary system evolves in the main sequence, the tidal friction will make the rotation and revolution approach to a closed state in a short time, but it takes a long time to attain a complete synchronization. After mass exchange started, the synchronous rotation can be changed more easily into the non-synchronous rotation for the semi-detached binaries. But for the contact binaries, the mass exchange is not strong enough to break the synchronization. The evolutionary tracks of the synchronization and non-synchronization models in the HR diagram are also compared with each other, and the result shows that for the non-synchronization model, the evolutionary curve of the primary star moves toward the direction of high luminosity and high effective temperature on the HR diagram at the mass exchange stage. Finally, by analyzing the statistical data of observations, it is found that the observed fact that the non-synchronous rotation exists in a period even longer than the tide-locking timescale can be explained by this model. © 2013 Elsevier B.V.

关键词： Binaries Close-stars Numerical Rotation-methods

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White dwarf accretion and type Ia supernovae

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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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