检索结果-内蒙古大学图书馆

arXiv 2019年

作者： Yang, Yi Hoeflich, Peter Baade, Dietrich Maund, Justyn R. Wang, Lifan Brown, Peter J. Stevance, Heloise F. Arcavi, Iair Burke, Jamison Cikota, Aleksandar Clocchiatti, Alejandro Gal-Yam, Avishay Graham, Melissa L. Hiramatsu, Daichi Hosseinzadeh, Griffin Howell, D. Andrew Jha, Saurabh W. McCully, Curtis Patat, Ferdinando Sand, David J. Schulze, Steve Spyromilio, Jason Valenti, Stefano Vinkao, Jozsef Wang, Xiaofeng Wheeler, J. Craig Yaron, Ofer Zhang, Jujia Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot76100 Israel Department of Physics Florida State University TallahasseeFL32306-4350 United States European Southern Observatory Karl-Schwarzschild-Str. 2 Garching b. Munchen85748 Germany Department of Physics and Astronomy University of Sheffield Hicks Building Hounsfield Road SheffieldS37RH United Kingdom George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy Texas A. & M. University 4242 TAMU College StationTX77843 United States Purple Mountain Observatory Chinese Academy of Sciences Nanjing210008 China Raymond and Beverly Sackler School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel Las Cumbres Observatory 6740 Cortona Drive Suite 102 GoletaCA93117-5575 United States Department of Physics University of California Santa BarbaraCA93106-9530 United States Physics Division Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Casilla 306 Santiago 22 Department of Astronomy University of Washington Box 351580 U.W. SeattleWA98195 United States Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States Department of Physics and Astronomy Rutgers State University of New Jersey 136 Frelinghuysen Rd. PiscatawayNJ08854 United States Center for Computational Astrophysics Flatiron Institute 162 5th Avenue New YorkNY10010 United States Steward Observatory University of Arizona 933 North Cherry Avenue Rm. N204 TucsonAZ85721-0065 United States Department of Physics University of California DavisCA95616 United States Konkoly Observatory MTA CSFK Konkoly Thege M. ut 15-17 Budapest1121 Hungary Department of Optics & Quantum Electronics University of Szeged Dom ter 9 Szeged6720 Hungary Department of Astronomy University of Texas at Austin AustinTX78712 United States Tsinghua University Beijing100084 Chinese Academy of Sciences

The non-detection of companion stars in Type Ia supernova (SN) progenitor systems lends support to the notion of double-degenerate (DD) systems and explosions triggered by the merging of two white dwarfs. This very asymmetric process should lead to a conspicuous polarimetric signature. By contrast, observations consistently find very low continuum polarization as the signatures from the explosion process largely dominate over the pre-explosion configuration within several days. Critical information about the interaction of the ejecta with a companion and any circumstellar matter is encoded in the early polarization spectra. In this study, we obtain spectropolarimetry of SN2018gv with the ESO Very Large Telescope at .13.6 days relative to the *** maximum light, or 5 days after the estimated explosion the earliest spectropolarimetric observations to date of any Type Ia SN. These early observations still show a low continuum polarization (-0.2%) and moderate line polarization (0.30 0.04% for the prominent Si II 6355 feature and 0.85 0.04% for the high-velocity Ca component). The high degree of spherical symmetry implied by the low line and continuum polarization at this early epoch is consistent with explosion models of delayed detonations and is inconsistent with the merger-induced explosion scenario. The dense UV and optical photometry and optical spectroscopy within the first 100 days after the maximum light indicate that SN2018gv is a normal Type Ia SN with similar spectrophotometric behavior to SN2011fe. Copyright © 2019, The Authors. All rights reserved.

关键词： Polarization

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GRANDMA Observations of SN 2023wrk, a Luminous Type Ia Supernova with Significant Unburned Carbon in the Outer Ejecta

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Research Notes of the AAS 2024年第10期8卷 273-273页

作者： Cristina Andrade Pierre-Alexandre Duverne Jialian Liu Felipe Navarete Abdelaziz E. Abdelaziz Mohamed Abdelkareem Ilmah Abdi Mohamed Aboueisha Christophe Adami Shabnam Agayeva Vova Aivazyan Leandro de Almeida Dalya Akl Sarah Antier Yvan Arnaud Saad A. Ata Wageeh A. Badawy Chunhai Bai Reda Bendary Zouhair Benkhaldoun Kevin Borrot Eric Broens Yongzhi Cai Olivier Clerget Wagner Corradi Michael W. Coughlin Nicolas Delaunoy Franky Dubois Jean-Grégoire Ducoin Eslam Elhosseiny Thomas M. Esposito Ali Esamdin Pascal Foulon Roland Foulon Michael Freeberg Charles Galdies Priyadarshini Gokuldass Bruno Guillet Gamal M. Hamed Bruno Haremza Patrice Hello Yasser Hendy Patrick Huth Raguli Inasaridze Abdusamatjan Iskandar Aziz Kaeouach Tarek M. Kamel Sergey Karpov Raymond Kneip Nino Kochiashvili Petri Kuossari Liping Li Xin Li Jinzhong Liu Markus Lorber Raouf H. Mabrouk Denis Marchais Elisabeth Maris Isabel Márquez Martin Mašek Roger Ménard Nicola Meneghelli Mike Mitchell Kanthanakorn Noysena Mohammad Odeh Wataru Ono Gérard Parent Bruce Parker Julien Peloton Adam Popowicz Thierry Pradier Stephen Price Oleksandra Pyshna Yodgor Rajabov Fadi Saibi Sophie Saibi Denis Saint-Gelais Nelio Sasaki Marc Serrau Masao Shimizu Ahmed Shokry Andrii Simon Oleksii Sokoliuk Ali Takey Manasanun Tanasan Yusuf Tillayev Giuseppe Di Tommaso Iara Tosta e Melo Damien Turpin Xiaofeng Wang Zhenyu Wang Ibrahim Zead Jujia Zhang School of Physics and Astronomy University of Minnesota Minneapolis MN 55455 USA Université Paris Cité CNRS Astroparticule et Cosmologie F-75013 Paris France Physics Department Tsinghua University Beijing 100084 People's Republic of China SOAR Telescope/NSF’s NOIRLab Avda Juan Cisternas 1500 1700000 La Serena Chile National Research Institute of Astronomy and Geophysics (NRIAG) 1 El-marsad St. 11421 Helwan Cairo Egypt Physics Department American University of Sharjah Sharjah UAE Aix Marseille Univ CNRS CNES LAM Marseille France N.Tusi Shamakhy Astrophysical Observatory Azerbaijan National Academy of Sciences settl.Y. Mammadaliyev AZ 5626 Shamakhy Azerbaijan E. Kharadze Georgian National Astrophysical Observatory Mt.Kanobili Abastumani 0301 Adigeni Georgia Laboratório Nacional de Astrofísica R. dos Estados Unidos 154—Nações Itajubá—MG 37504-364 Brazil Université Côte d’Azur Observatoire de la Côte d’Azur CNRS Boulevard de l’Observatoire 06304 Nice France Unistellar Network France Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi Xinjiang 830011 People's Republic of China Oukaimeden Observatory High Energy Physics and Astrophysics Laboratory FSSM Cadi Ayyad University Morocco GRANDMA: Kilonova-Catcher Vereniging Voor Sterrenkunde Balen-Neetlaan 18A B-2400 Mol Belgium Yunnan Observatories Chinese Academy of Sciences Kunming 650216 People's Republic of China International Centre of Supernovae Yunnan Key Laboratory Kunming 650216 People's Republic of China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650216 People's Republic of China Adonis Observatory (private obs.) Poelkapellestraat 57 Langemark 8920 Belgium CPPM Aix Marseille Univ CNRS/IN2P3 CPPM Marseille France SETI Institute Carl Sagan Center 339 Bernardo Ave Suite 200 Mountain View CA 94043 USA Unistellar 5 allée Marcel Leclerc bâtiment B Marseille 13008 France Department of Astronomy University of

First detected on 2023 November 4 by the Gravitational-wave Optical Transient Observer, SN 2023wrk is a Type Ia Supernova at 40 Mpc, with significant unburned carbon in the outer ejecta. In this note, we present photometric and spectroscopic observations and analysis conducted by the Global Rapid Advanced Network Devoted to the Multi-messenger Addict over a 115 days period, which includes 78 days of measurements. The observations were contributed by both amateur and professional astronomers. J. Liu et al. analyzed the physical processes involved, and compared the evolution of color and spectral lines. We conclude that SN 2023wrk is the second 1999aa-like object with strong carbon absorption lines that has ever been found, which enriches our understanding of the subclass of 1999aa-like SNe.

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Bright mini-outburst ends the 12−year long activity of the black hole candidate swift J1753.5−0127

arXiv

引用

arXiv 2019年

作者： Zhang, G.-B. Bernardini, F. Russell, D.M. Gelfand, J.D. Lasota, J.-P. Al Qasim, A. AlMannaei, A. Koljonen, K.I.I. Shaw, A.W. Lewis, F. Tomsick, J.A. Plotkin, R.M. Miller-Jones, J.C.A. Maitra, D. Homan, J. Charles, P.A. Kobel, P. Perez, D. Doran, R. Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650216 China Center for Astronomical Mega-Science CAS Beijing100012 China New York University Abu Dhabi P.O. Box 129188 Abu Dhabi United Arab Emirates INAF − Osservatorio Astronomico di Roma via Frascati 33 Monteporzio Catone RomaI-00040 Italy INAF − Osservatorio Astronomico di Capodimonte Salita Moiariello 16 NapoliI-80131 Italy Center for Cosmology and Particle Physics New York University Meyer Hall of Physics 4 Washington Place New YorkNY10003 United States Institut d’Astrophysique de Paris CNRS et Sorbonne Universités UPMC Paris 06 UMR 7095 98bis Bd Arago Paris75014 France Nicolaus Copernicus Astronomical Center Bartycka 18 Warsaw00-716 Poland Mullard Space Science Laboratory University College London Holmbury St. Mary Dorking SurreyRH5 6NT United Kingdom University of Turku Väisäläntie 20 Piikkiö21500 Finland Aalto University Metsähovi Radio Observatory PO Box 13000 AaltoFI-00076 Finland Department of Physics University of Alberta 4-181 CCIS EdmontonABT6G 2E1 Canada Faulkes Telescope Project School of Physics and Astronomy Cardiff University The Parade CardiffCF24 3AA United Kingdom Astrophysics Research Institute Liverpool John Moores University 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Space Sciences Laboratory University of California 7 Gauss Way BerkeleyCA94720-7450 United States International Centre for Radio Astronomy Research Curtin University GPO Box U1987 PerthWA6845 Australia Department of Physics and Astronomy Wheaton College NortonMA02766 United States Eureka Scientific Inc. 2452 Delmer Street OaklandCA94602 United States SRON Netherlands Institute for Space Research Sorbonnelaan 2 Utrecht3584 CA Netherlands Department of Physics & Astronomy University of Southampton SouthamptonSO17 1BJ United Kingdom Gymnase du Bugnon-Sévelin Avenue de Sévelin 44 Lausanne1004 Switzerland NUCLIO - N

We present optical, UV and X-ray monitoring of the short orbital period black hole X-ray binary candidate Swift J1753.5–0127, focusing on the final stages of its 12−year long outburst that started in 2005. From September 2016 onward, the source started to fade and within three months, the optical flux almost reached the quiescent level. Soon after that, using a new proposed rebrightening classification method we recorded a mini-outburst and a reflare in the optical light curves, peaking in February (V-17.0) and May (V-17.9) 2017, respectively. Remarkably, the mini-outburst has a peak flux consistent with the extrapolation of the slow decay before the fading phase preceding it. The following reflare was fainter and shorter. We found from optical colors that the temperature of the outer disk was - 11,000 K when the source started to fade rapidly. According to the disk instability model, this is close to the critical temperature when a cooling wave is expected to form in the disk, shutting down the outburst. The optical color could be a useful tool to predict decay rates in some X-ray transients. We notice that all X-ray binaries that show mini-outbursts following a main outburst are short orbital period systems ( Copyright © 2019, The Authors. All rights reserved.

关键词： Stars

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SN 2014J in M82: New insights on the spectral diversity of type Ia supernovae

arXiv

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arXiv 2018年

作者： Zhang, Kaicheng Wang, Xiaofeng Zhang, JuJia Zhang, Tianmeng Benetti, S. Elias-Rosa, N. Huang, Fang Lin, Han Li, Linyi Li, Wenxiong Ochner, P. Pastorello, A. Rui, Liming Tartaglia, L. Tomasella, L. Siviero, A. Munari, U. Terreran, G. Song, Hao Taubenberger, S. Wheeler, J. Craig Xiang, Danfeng Zhao, Xulin Li, Hongbin Bai, Jinming Jiang, Xiaojun Shi, Jianrong Wu, Zhenyu Tsinghua University Beijing100084 China Department of Astronomy University of Texas at Austin AustinTX78712-1205 United States Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory of Optical Astronomy National Astronomical Observatory of China Chinese Academy of Sciences Beijing100012 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China INAF - Osservatorio Astronomico di Padova vicolo dell’Osservatorio 5 PadovaI-35122 Italy Department of Astronomy School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Dipartimento di Fisica e Astronomia Università di Padova via Marzolo 8 PadovaI-35131 Italy Department of Astronomy and The Oskar Klein Centre AlbaNova University Center Stockholm University StockholmSE-106 91 Sweden Department of Physics and Astronomy Northwestern Unive European Southern Observatory Karl-Schwarzschild-Str. 2 Garching85748 Germany Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str. 1 Garching85748 Germany School of Science Tianjin University of Technology Tianjin300384 China

We present extensive spectroscopic observations for one of the closest type Ia supernovae (SNe Ia), SN 2014J discovered in M82, ranging from 10.4 days before to 473.2 days after B-band maximum light. The diffuse interstellar band (DIB) features detected in a high-resolution spectrum allow an estimate of line-of-sight extinction as Av ∼1.9±0.6 mag. Spectroscopically, SN 2014J can be put into the high-velocity (HV) subgroup in Wang’s classification with a velocity of Si ii λ 6355 at maximum light of v0 = 1.22±0.01×104 km s−1, but has a low velocity gradient (LVG, following Benetti’s classification) of vÛ = 41±2 km s−1 day−1, which is inconsistent with the trend that HV SNe Ia generally have larger velocity gradients. We find that the HV SNe Ia with LVGs tend to have relatively stronger Si iii (at ∼4400 Å) absorptions in early spectra, larger ratios of S ii λ 5468 to S ii λ 5640, and weaker Si ii 5972 absorptions compared to their counterparts with similar velocities but high velocity gradients. This shows that the HV+LVG subgroup of SNe Ia may have intrinsically higher photospheric temperature, which indicates that their progenitors may experience more complete burning in the explosions relative to the typical HV SNe Ia. Copyright © 2018, The Authors. All rights reserved.

关键词： Supernovae

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Quiescent photometric modulations of two low-inclination cataclysmic variables KZ Gem and TW Vir

arXiv

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arXiv 2017年

作者： Dai, Zhibin Szkody, Paula Taani, Ali Garnavich, Peter M. Kennedy, Mark Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China University of Washington SeattleWA98195 United States Applied Sciences Department Aqaba University College Al-Balqa' Applied University P.O. Box 1199 Aqaba77110 Jordan University of Notre Dame Notre DameIN46556 United States Department of Physics University College Cork Cork Ireland

Aims. The quiescent periodic photometric modulations of two low-inclination cataclysmic variables observed in Kepler K2 Campaigns 0 and 1, KZ Gem and TW Vir, are investigated. Methods. A phase-correcting method was successfully used to detect the orbital modulations of KZ Gem and TW Vir and improve their orbital periods. The light curve morphologies of both CVs were further analyzed by defining flux ratios and creating colormaps. Results. KZ Gem shows ellipsoidal modulations with an orbital period of 0.22242(1) day, twice the period listed in the updated RK catalogue (Edition 7.24). With this newly determined period, KZ Gem is no longer a CV in the period gap, but a long-period CV. A part of the quiescent light curve of TW Vir that had the highest stability was used to deduce its improved orbital period of 0.182682(3) day. The flat patterns shown in the colormaps of the flux ratios for KZ Gem demonstrate the stability of their orbital modulations, while TW Vir show variable orbital modulations during the K2 datasets. In TW Vir, the single versus double-peaked nature of the quiescent orbital variations before and after superoutburst may be related to the effect of the superoutburst on the accretion disk. Copyright © 2017, The Authors. All rights reserved.

关键词： Photometry

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NEUTRAL CARBON EMISSION IN LUMINOUS INFRARED GALAXIES THE [Ci] LINES AS TOTAL MOLECULAR GAS TRACERS

arXiv

引用

arXiv 2017年

作者： Jiao, Qian Zhao, Yinghe Zhu, Ming Lu, Nanyao Gao, Yu Zhang, Zhi-Yu Beijing100012 China Key Laboratory of Radio Astronomy CAS Beijing100012 China University of Chinese Academy of Sciences Beijing100012 China Yunnan Observatories CAS Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650011 China Center for Astronomical Mega-Science CAS 20A Datun Road Chaoyang District Beijing100012 China Purple Mountain Observatory CAS Nanjing210008 China Camino El Observatorio 1515 Las Condes Santiago Chile Key Laboratory of Radio Astronomy CAS Nanjing210008 China Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom ESO Karl Schwarzschild Strasse 2 Garching MunichD-85748 Germany

We present a statistical study on the (formula presented) lines (hereafter [C i] (1−0) and [C i] (2−1), respectively) and the CO (1−0) line for a sample of (ultra)luminous infrared galaxies [(U)LIRGs]. We explore the correlations between the luminosities of CO (1−0) and [C i] lines, and find that L′CO(1−0) correlates almost linearly with both (formula presented), suggesting that [C i] lines can trace total molecular gas mass at least for (U)LIRGs. We also investigate the dependence of (formula presented) and (formula presented)on the far-infrared color of 60-to-100 µm, and find non-correlation, a weak correlation and a modest correlation, respectively. Under the assumption that these two carbon transitions are optically thin, we further calculate the [C i] line excitation temperatures, atomic carbon masses, and the mean [C i] line flux-to-H2 mass conversion factors for our sample. The resulting H2 masses using these [C i]-based conversion factors roughly agree with those derived from L′CO(1−0) and CO-to-H2 conversion factor. Copyright © 2017, The Authors. All rights reserved.

关键词： Molecules

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Studies for slowly rotating asteroids (168) Sibylla and (346) Hermentaria

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Proceedings of the International Astronomical Union 2016年第S318期10卷 185-192页

作者： Wang, Xiaobin Muinonen, Karri Han, Xianming L. Kwok, Chi-Tai Yunnan Observatories CAS P.O. Box 110 Kunming Yunnan Province 650011 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming 650011 China Department of Physics University of Helsinki Gustaf Hällströmin katu 2a P.O. Box 64 U. Helsinki FI-00014 Finland Finnish Geospatial Research Institute Geodeetinrinne 2 Masala FI-02430 Finland Department of Physics and Astronomy Butler University Indianapolis IN United States Ho Koon Nature Education Cum Astronomical Centre Sik Sik Yuen Hong Kong

Studies for spin parameters and shapes of asteroids provide us with important information about the interior structure of asteroids and the physical processes they have undergone. A large sample of basic physical parameters can help us also understand the evolution of asteroids. There is scarce information for slowly-rotating larger asteroids because more effort is required for observing them. Because of this, we have established an international collaboration to study slowly-rotating asteroids. As the first step of this project, we have observed asteroids (168) Sibylla and (346) Hermentaria in 2014 and 2015 using several telescopes located in China, Chile, and U.S.A. Combining previous photometric data with our new data, we have performed preliminary analyses and obtained spin parameters and shapes with their uncertainties for these two slowly-rotating asteroids for the first time, using the convex inversion method and the virtual photometry Monte Carlo method. A pair of pole solutions for (168) Sibylla are found around (4.3°, 53.5°) and (183.5°, 52.6°) with a period of 47.0000 h. We have found that the shape of Sibylla resembles an oblate spheroid. For (346) Hermentaria, we have also found a pair of pole solutions around (134.5°, 16.7°) and (321.5°, 14.5°) with comparable rms-values with a spin period of about 17.79000 h, and a shape resembling a prolate spheroid. Copyright © 2016 International Astronomical Union.

关键词： asteroids methods: data analysis methods: numerical methods: statistical Minor planets radiative transfer scattering solar system: general techniques: photometric

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Search for Exoplanets around Northern Circumpolar Stars II. The Detection of Radial Velocity Variations in M Giant Stars HD 36384, HD 52030, and HD 208742

arXiv

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arXiv 2017年

作者： Lee, Byeong-Cheol Jeong, Gwanghui Park, Myeong-Gu Han, Inwoo Mkrtichian, David E. Hatzes, Artie P. Gu, Shenghong Bai, Jinming Lee, Sang-Min Oh, Hyeong-Il Kim, Kang-Min Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon305-348 Korea Republic of Astronomy and Space Science Major Korea University of Science and Technology Gajeong-ro Yuseong-gu Daejeon305-333 Korea Republic of Department of Astronomy and Atmospheric Sciences Kyungpook National University Daegu702-701 Korea Republic of National Astronomical Research Institute of Thailand Chiang Mai50200 Thailand Crimean Astrophysical Observatory Taras Shevchenko National University of Kyiv Nauchny Crimea98409 Ukraine Sternwarte 5 Tautenburg07778 Germany Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China

We present the detection of long-period RV variations in HD 36384, HD 52030, and HD 208742 by using the high-resolution, fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) for the precise radial velocity (RV) survey of about 200 northern circumpolar stars. Analyses of RV data, chromospheric activity indicators, and bisector variations spanning about five years suggest that the RV variations are compatible with planet or brown dwarf companions in Keplerian motion. However, HD 36384 shows photometric variations with a period very close to that of RV variations as well as amplitude variations in the weighted wavelet Z-transform (WWZ) analysis, which argues that the RV variations in HD 36384 are from the stellar pulsations. Assuming that the companion hypothesis is correct, HD 52030 hosts a companion with minimum mass 13.3 MJup orbiting in 484 days at a distance of 1.2 AU. HD 208742 hosts a companion of Copyright © 2017, The Authors. All rights reserved.

关键词： Orbits

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Hubble Space Telescope Ultraviolet Light Curves Reveal Interesting Properties of CC Sculptoris and RZ Leonis

arXiv

引用

arXiv 2017年

作者： Szkody, Paula Mukadam, Anjum S. Toloza, Odette Gänsicke, Boris T. Dai, Zhibin Pala, Anna F. Waagen, Elizabeth O. Godon, Patrick Sion, Edward M. Department of Astronomy University of Washington Box 351580 SeattleWA98195 United States Apache Point Observatory Astrophysical Research Consortium Department of Physics University of Warwick CoventryCV4 7AL United Kingdom Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China AAVSO 48 Bay State Rd CambridgeMA02138 Department of Astrophysics and Planetary Science Villanova University VillanovaPA19085 United States

Time-tag ultraviolet data obtained on the Hubble Space Telescope in 2013 reveal interesting variability related to the white dwarf spin in the two cataclysmic variables RZ Leo and CC Scl. RZ Leo shows a period at 220 s and its harmonic at 110 s, thus identifying it as a likely Intermediate Polar (IP). The spin signal is not visible in a short single night of ground based data in 2016, but the shorter exposures in that dataset indicate a possible partial eclipse. The much larger UV amplitude of the spin signal in the known IP CC Scl allows the spin of 389 s, previously only seen at outburst, to be visible at quiescence. Spectra created from the peaks and troughs of the spin times indicate a hotter temperature of several thousand degrees during the peak phases, with multiple components contributing to the UV light. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

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Monitor variability of millimeter lines in IRC+10216

arXiv

引用

arXiv 2017年

作者： He, J.H. -Trung, Dinh-V Hasegawa, T.I. Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Chinese Academy of Sciences South America Center for Astronomy China-Chile Joint Center for Astronomy Camino El Observatorio #1515 Las Condes Santiago Chile Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Institute of Physics Vietnam Academy of Science and Technology 10 DaoTan BaDinh Hanoi Viet Nam Academia Sinica Astronomy and Astrophysics AS/NTU. No.1 Sec. 4 Roosevelt Rd Taipei10617 Taiwan

A single dish monitoring of millimeter maser lines SiS J=14-13 and HCNv2 = 1f J=3-2 and several other rotational lines is reported for the archetypal carbon star IRC+10216. Relative line strength variations of 5%∼30% are found for eight molecular line features with respect to selected reference lines. Definite line-shape variation is found in limited velocity intervals of the SiS and HCN line profiles. The asymmetrical line profiles of the two lines are mainly due to the varying components. Their dominant varying components of the line profiles have similar periods and phases as the IR light variation, although both quantities show some degree of velocity dependence;there is also variability asymmetry between the blue and red line wings of both lines. Combining the velocities and amplitudes with a wind velocity model, we suggest that the line profile variations are due to SiS and HCN masing lines emanating from the wind acceleration zone. The possible link of the variabilities to thermal, dynamical and/or chemical processes within or under this region is also discussed. Copyright © 2017, The Authors. All rights reserved.

关键词： Masers

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