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arXiv 2020年

作者： Zuo, Wenwen Wu, Xue-Bing Fan, Xiaohui Green, Richard Yi, Weiming Schulze, Andreas Wang, Ran Bian, Fuyan Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Department of Astronomy School of Physics Peking University Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Steward Observatory University of Arizona TucsonAZ85721 United States Yunnan Observatories Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China National Astronomical Observatory of Japan Mitaka181-8588 Japan European Southern Observatory Alonso de CÃşrdova 3107 Casilla 19001 Vitacura Santiago 19 Chile

Using a high luminosity (Lbol ∼ 1047.5 − 1048.3 erg s−1), high redshift (3.2 BH). The median logarithm of the CIV- and Hβ-based MBH ratios is 0.110 dex with the scatter of 0.647 dex. The CIV-to-Hβ BH mass differences are significantly correlated with the CIV FWHMs, blueshifts and asymmetries. Corrections of the CIV FWHM using the blueshift and asymmetry reduce the scatter of the mass differences by ∼ 0.04-0.2 dex. Quasars in our sample accrete at the Eddington ratio REDD > 0.3 and cover a considerable range of blueshifts, with 18/19 of the quasars showing CIV blueshifts (with the median value of 1126 km s−1) and 14/19 of the quasars showing CIV blueshifts larger than 500 km s−1. It suggests that not all quasars with high Eddington ratios show large blueshifts. The Baldwin effect between the CIV rest-frame equivalent width (REW) and the continuum luminosity at 1350 Å is not seen, likely due to the limited luminosity range of our sample. We find a lack of flux in the red wing of the composite spectrum with larger CIV blueshift, and detect a higher ratio of [OIII] quasars with REW[OIII] > 5 Å in the subsample with lower CIV blueshift. It is more likely that they are caused by the combination of the Eddington ratio and the orientation effect. Copyright © 2020, The Authors. All rights reserved.

关键词： Galaxies

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GRB x-ray flare properties among different GRB subclasses

arXiv

引用

arXiv 2019年

作者： Liu, Chuanxi Mao, Jirong Yunnan Observatories Chinese Academy of Sciences Yunnan Province Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China

Gamma-ray bursts (GRBs) can be divided into three subclasses: X-ray flash (XRF), X-ray rich (XRR), and classical GRB (C-GRB). An X-ray flare is the rebrightening emission shown in the early X-ray afterglow of some GRBs. In this paper, we comprehensively examine the X-ray flare properties among XRF, XRR, and C-GRB subclasses. We utilize the XRF, XRR, and C-GRB subclass samples obtained from the Swift-BAT3 catalog, and the X-ray flare observational properties are collected from Falcone et al., Chincarini et al., and Yi et al. We find that XRFs and XRRs have more bright X-ray flares than C-GRBs. The ratio of the X-ray flare fluence to the prompt emission fluence has different distributions between XRF and C-GRB subclasses. The linear correlation between the duration and the peak time of the X-ray flares is also different between XRF and C-GRB subclasses. We are inclined to identify the GRBs with the bright X-ray flares as XRFs or XRRs. We discuss some issues that are related to the XRF/XRR/C-GRB classification. We also caution the selection effects and the instrument bias in our investigation. Large samples are required in the future to further confirm our results. Copyright © 2019, The Authors. All rights reserved.

关键词： Gamma rays

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evolution of A Peculiar Type Ibn Supernova SN 2019wep

arXiv

引用

arXiv 2022年

作者： Gangopadhyay, Anjasha Misra, Kuntal Hosseinzadeh, Griffin Arcavi, Iair Pellegrino, Craig Wang, Xiaofeng Howell, D. Andrew Burke, Jamison Zhang, Jujia Kawabata, Koji Singh, Mridweeka Dastidar, Raya Hiramatsu, Daichi McCully, Curtis Mo, Jun Chen, Zhihao Xiang, Danfeng Hiroshima Astrophysical Science Centre Hiroshima University 1-3-1 Kagamiyama Hiroshima Higashi-Hiroshima739-8526 Japan Aryabhatta Research Institute of Observational Sciences Manora Peak Nainital 263 002 India Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721 United States The School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel CIFAR Azrieli Global Scholars program CIFAR Toronto Canada Las Cumbres Observatory 6740 Cortona Drive Suite 102 GoletaCA93117-5575 United States Department of Physics University of California Santa BarbaraCA93106-9530 United States Physics Department Tsinghua Center for Astrophysics Tsinghua University China Beijing Planetarium Beijing Academy of Sciences Beijing100044 China Yunnan Astronomical Observatory of China Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650216 China Indian Institute of Astrophysics 2nd Block 100 Feet Rd Koramangala Karnataka Bengaluru560034 India Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of Millennium Institute of Astrophysics Nuncio Monsenor Sótero Sanz 100 Providencia Santiago8320000 Chile

We present a high-cadence short term photometric and spectroscopic monitoring campaign of a type Ibn SN 2019wep, which is one of the rare SN Ibn after SNe 2010al and 2019uo to display signatures of flash ionization (He II, C III, N III). We compare the decline rates and rise time of SN 2019wep with other SNe Ibn and fast transients. The post-peak decline in all bands (0.1 mag d−1) are consistent with SNe Ibn but less than the fast transients. On the other hand, the ∆m15 values are slightly lower than the average values for SNe Ibn but consistent with the fast transients. The rise time is typically shorter than SNe Ibn but longer than fast transients. SN 2019wep lies at the fainter end of SNe Ibn but possesses an average luminosity amongst the fast transients sample. The peculiar color evolution places it between SNe Ib and the most extreme SNe Ibn. The bolometric light curve modelling shows resemblance with SN 2019uo with ejecta masses consistent with SNe Ib. SN 2019wep belongs to the "P cygni" sub-class of SNe Ibn and shows faster evolution in line velocities as compared to the "emission" sub-class. The post-maximum spectra show close resemblance with ASASSN-15ed hinting it to be of SN Ib nature. The low He I CSM velocities and residual Hα further justifies it and gives evidence of an intermittent progenitor between WR and LBV star. Copyright © 2022, The Authors. All rights reserved.

关键词： Photometry

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CONTACT BINARIES AT THE SHORT PERIOD CUT-OFF I. STATISTICS AND THE FIRST PHOTOMETRIC INVESTIGATIONS OF TEN TOTALLY ECLIPSING SYSTEMS

arXiv

引用

arXiv 2019年

作者： Li, Kai Xia, Qi-Qi Michel, Raul Hu, Shao-Ming Guo, Di-Fu Gao, Xing Chen, Xu Gao, Dong-Yang Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment Institute of Space Sciences Shandong University Weihai264209 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Observatorio Astronómico Nacional Instituto de Astronomía Universidad Nacional Autónoma de México Apartado Postal 877 EnsenadaB.C.22830 Mexico Xinjiang Astronomical Observatory 150 Science 1-Street Urumqi830011 China

The period distribution of contact binaries exhibits a very sharp short period cut-off at 0.22 days. In order to provide valuable information on this short period limit, we observed ten totally eclipsing contact binaries with orbital periods near this cut-off. By detailed analysis using W-D code, we determined that two of these systems are A-subtype contact binaries while the others are W-subtype contact binaries and all the targets show shallow contact configurations. Half of the targets exhibit stellar spot activity and four of them have third light. A statistical work on well studied USPCBs was carried out, and physical parameters of fifty-five USPCBs were obtained. Some common properties for these systems were derived. Due to the study of the period-color diagram of USPCBs, we found that the period-color relation of USPCBs is different from other W UMa type contact binaries and USPCBs are metal poor old stars. In addition, the evolutionary states of these systems were discussed by constructing the color-density diagram. We derived that the evolutionary states of the two components of USPCBs show identical characteristics of other contact binaries despite slower evolutionary status caused by smaller mass. We suggested that both the fully convective limit claimed by Rucinski (1992) and the AML theory recommended by Stepien (2006) can produce the short period cut-off and a tertiary companion is very important during the formation of the short period contact binaries by removing angular momentum from the host eclipsing pairs under certain circumstances. Copyright © 2019, The Authors. All rights reserved.

关键词： Stars

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The escape of hydrogen-rich atmosphere of exoplanet: mass loss rates and the absorptions of stellar lyman α

arXiv

引用

arXiv 2019年

作者： Yan, D.D. Guo, J.H. Yunnan Observatories Chinese Academy of Sciences P.O. Box 110 Kunming650011 China Yunnan Observatories Chinese Academy of Sciences P.O. Box 110 Kunming650011 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650011 China

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A Superluminous Supernova Lightened by Collisions with Pulsational Pair-instability Shells

arXiv

引用

arXiv 2023年

作者： Lin, Weili Wang, Xiaofeng Yan, Lin Gal-Yam, Avishay Mo, Jun Brink, Thomas G. Filippenko, Alexei V. Xiang, Danfeng Lunnan, Ragnhild Zheng, Weikang Brown, Peter Kasliwal, Mansi Fremling, Christoffer Blagorodnova, Nadejda Mirzaqulov, Davron Ehgamberdiev, Shuhrat A. Lin, Han Zhang, Kaicheng Zhang, Jicheng Yan, Shengyu Zhang, Jujia Chen, Zhihao Deng, Licai Wang, Kun Xiao, Lin Wang, Lingjun Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 China Purple Mountain Observatory Chinese Academy of Science Nanjing210008 China Caltech Optical Observatories California Institute of Technology PasadenaCA91125 United States Department of Particle Physics and Astrophysics Weizmann Institute of Science 234 Herzl St. Rehovot76100 Israel Department of Astronomy University of California BerkeleyCA94720-3411 United States The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-106 91 Sweden Department of Physics and Astronomy Texas A&M University 4242 TAMU College StationTX77843 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy United States Division of Physics Mathematics and Astronomy California Institute of Technology PasadenaCA91125 United States c. Martí i Franquès 1 Barcelona08028 Spain c. Martí i Franquès 1 Barcelona08028 Spain c. Gran Capità 2-4 Barcelona08034 Spain Ulugh Beg Astronomical Institute Uzbekistan Academy of Sciences Tashkent100052 Uzbekistan National University of Uzbekistan Tashkent100174 Uzbekistan Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Department of Astronomy Beijing Normal University Beijing China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Department of Astronomy China West Normal University Nanchong China CAS Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing China Department of Physics College of Physical Sciences and Technology Hebei University Wusidong Road 180 Baoding071002 C

Superluminous supernovae are among the most energetic stellar explosions in the Universe, but their energy sources remain an open question. Here we present long-term observations of one of the closest examples of the hydrogen-poor subclass (SLSNe-I), SN 2017egm, revealing the most complicated known luminosity evolution of SLSNe-I. Three distinct post-peak bumps were recorded in its light curve collected at about 100–350 days after maximum brightness, challenging current popular power models such as magnetar, fallback accretion, and interaction between ejecta and a circumstellar shell. However, the complex light curve can be well modelled by successive interactions with multiple circumstellar shells with a total mass of about 6.8–7.7 M☉. In this scenario, large energy deposition from interaction-induced reverse shocks results in ionization of neutral oxygen in the supernova ejecta and hence a much lower nebular-phase line ratio of [O I] λ6300/([Ca II] + [O II]) λ7300 (∼ 0.2) compared with that derived for other superluminous and normal stripped-envelope SNe. The pre-existing multiple shells indicate that the progenitor of SN 2017egm experienced pulsational mass ejections triggered by pair instability within 2 years before explosion, in robust agreement with theoretical predictions for a pre-pulsation helium-core mass of 48–51 M☉ © 2023, CC BY.

关键词： Supernovae

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The rate of period change in DAV stars

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Research in Astronomy and Astrophysics 2017年第7期17卷 11-24页

作者： Yan-Hui Chen Cai-Yun Ding Wei-Wei Na Hong Shu Institute of Astrophysics Chuxiong Normal University School of Physics and Electronical Science Chuxiong Normal University Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences School of Physics and Electronic Engineering Yuxi Normal University

Grids of DAV star models are evolved by WDEC, taking the element diffusion effect into account. The grid parameters are hydrogen mass log（MH/M＊）, helium mass log（MHe/M＊）, stellar mass M＊and effective temperature T_（eff） for DAV stars. The core compositions are from white dwarf models evolved by MESA. Therefore, DAV star models evolved by WDEC have historically viable core compositions. Based on those DAV star models, we studied the rate of period change（P˙（k）） for different values of H, He, M_＊and Teff. The results are consistent with previous work. Two DAV stars G117-B15A and R548 have been observed for around 40 years. The rates of period change of two large-amplitude modes were obtained through the O-C method. We conducted an asteroseismological study on the two DAV stars and then obtained a best-fitting model for each star. Based on the two best-fitting models,the mode identifications（l, k） of the observed modes for G117-B15A and R548 are consistent with previous work. Both the observed modes and the observedP˙ s can be fitted by calculated ones. The results indicate that our method of evolving DAV star models is feasible.

关键词： stars oscillations （including pulsations） - stars individual （G117-B 15A and R548） -white dwarfs

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Populations of accreting white dwarfs

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Proceedings of the International Astronomical Union 2019年第S343期14卷 371-372页

作者： Chen H.-L. Woods T.E. Yungelson L. Gilfanov M. Han Z. Yunnan Observatories CAS Kunming 650011 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming 650011 China Center for Astronomical Mega-Science Chinese Academy of Science Beijing 100012 China Institute of Gravitational Wave Astronomy School of Physics and Astronomy University of Birmingham Birmingham B15 2TT United Kingdom Institute of Astronomy RAS 48 Pyatnitskaya Str. Moscow 119017 Russian Federation Max Planck Institute for Astrophysics Karl-Schwarzschild-Str. 1 Garching b. München 85741 Germany Space Research Institute of Russian Academy of Sciences Profsoyuznaya 84/32 Moscow 117997 Russian Federation

Using a hybrid binary population synthesis approach, we modelled the formation and evolution of populations of accreting white dwarfs (WDs) for differing star formation histories. We found that the delay time distribution of SNe Ia in the single degenerate scenario is inconsistent with observations. Additionally, we found that our predicted X-ray and UV emission of populations of accreting WDs are consistent with the X-ray luminosities of early-type galaxies observed by Chandra and the HeII 4686 Å/Hβ line ratio measured in stacked SDSS spectra of passively evolving galaxies. Moreover, we found that the majority of current novae in elliptical-like galaxies have low-mass WDs, long decay times, long recurrence periods and are relatively faint. In contrast, the majority of current novae in spiral-like galaxies have massive WDs, short decay times, short recurrence periods and are relatively bright. Our predicted distribution of mass-loss timescales in an M31-like galaxy is consistent with observations for Andromeda. © International Astronomical Union 2019.

关键词： cataclysmic variables stars:novae white dwarfs

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Performance of the Stellar Abundances and atmospheric Parameters Pipeline adapted for M dwarfs I. Atmospheric parameters from the spectroscopic module

arXiv

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arXiv 2025年

作者： Olander, Terese Gent, Matthew R. Heiter, Ulrike Kochukhov, Oleg Bergemann, Maria Magg, Ekaterina Cassisi, Santi Kovalev, Mikhail Morel, Thierry Miller, Nicola J. Souto, Diogo Shan, Yutong Rojas-Ayala, Bárbara Delgado-Mena, Elisa Wang, Haiyang S. Department of Physics and Astronomy Uppsala University Box 516 UppsalaSE-751 20 Sweden Max Planck Institute for Astronomy Heidelberg69117 Germany Institut de Recherche en Astrophysique et Planétologie Université de Toulouse CNRS IRAP UMR 5277 14 Avenue Edouard Belin Toulouse31400 France INAF Osservatorio Astronomico d’Abruzzo Via M. Maggini s/n Teramo64100 Italy INFN Sezione di Pisa Largo Pontecorvo 3 Pisa56127 Italy Yunnan Observatories China Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Institute Université de Liège Quartier Agora Allée du 6 Août 19c Bât. B5c LiègeB4000 Belgium Departamento de Física Universidade Federal de Sergipe Av. Marcelo Deda Chagas S/N SE São CristóvãoCep 49.107-230 Brazil Centre for Planetary Habitability Department of Geosciences University of Oslo Sem Sælands Vei 2b Oslo0315 Norway Institut für Astrophysik Georg-August-Universität Friedrich-Hund-Platz 1 Göttingen37077 Germany Instituto de Alta Investigación Universidad de Tarapacá Casilla 7D Arica Chile CAUP Universidade do Porto Rua das Estrelas PortoPT4150-762 Portugal CSIC-INTA Camino Bajo del Castillo s/n Madrid Villanueva de la Cañada28692 Spain Center for Star and Planet Formation Globe Institute The University of Copenhagen Øster Voldgade 5-7 København K1350 Denmark

Context. M dwarfs are important targets in the search for Earth-like exoplanets due to their small masses and low luminosities. Several ongoing and upcoming space missions are targeting M dwarfs for this reason, and the ESA Plato mission is one of these. Aims. In order to fully characterise a planetary system the properties of the host star must be known. For M dwarfs we can derive effective temperature, surface gravity, metallicity, and abundances of various elements from spectroscopic observations in combination with photometric data. Methods. The Stellar Abundances and atmospheric Parameters Pipeline (SAPP) has been developed to serve as a prototype for one of the stellar science softwares within the Plato consortium. The pipeline combines results from a spectroscopy, a photometry, an interferometry, and an asteroseismology module to derive stellar parameters for FGK-type stars. We have modified the pipeline to be able to analyse the M dwarf part of the Plato target sample. The current version of the pipeline for M dwarfs mostly relies on spectroscopic observations. The module processing these data is based on the machine learning algorithm The Payne and fits a grid of model spectra to an observed spectrum to derive effective temperature and metallicity. We use spectra in the H-band, as the near-infrared region is beneficial for M dwarfs because there are fewer molecular lines and they are brighter in this wavelength region than in the optical. A method based on synthetic spectra was developed for the continuum normalisation of the spectra, taking into account the pseudo-continuum formed by numerous lines of the water molecule. Photometry is used to constrain the surface gravity. Results. We tested the modified SAPP on spectra of M dwarfs from the APOGEE survey. Our validation sample of 26 stars includes stars with interferometric observations and binaries. We found a good agreement between our derived values and reference values from a range of previous studies.

关键词： Photometers

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SN 2015bf: A fast declining type II supernova with flash-ionised signatures

arXiv

引用

arXiv 2021年

作者： Lin, Han Wang, Xiaofeng Zhang, Jujia Lin, Weili Mo, Jun Filippenko, Alexei V. Zheng, WeiKang Brown, Peter J. Xiang, Danfeng Huang, Fang Cai, Yongzhi Zhang, Tianmeng Li, Xue Rui, Liming Zhang, Xinghan Sai, Hanna Zhao, Xulin Graham, Melissa L. Shivvers, I. Halevi, G. Yuk, H. Brink, Thomas G. Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Sciences and Technology Beijing100044 China Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China 20A Datun Road Chaoyang District Beijing100012 China Department of Astronomy University of California BerkeleyCA94720-3411 United States Miller Institute for Basic Research in Science University of California BerkeleyCA94720-3411 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Texas A&M University Department of Physics and Astronomy 4242 TAMU College StationTX77843 United States Department of Astronomy Shanghai Jiao Tong University Shanghai200240 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China School of Science Tianjin University of Technology Tianjin300384 China DiRAC Institute Department of Astronomy University of Washington Box 351580 SeattleWA98195 United States Homer L. Dodge Department of Physics and Astronomy University of Oklahoma 440 W. Brooks St. NormanOK73019 United States

We present optical and ultraviolet photometry, as well as optical spectra, for the type II supernova (SN) 2015bf. Our observations cover the phases from ∼ 2 to ∼ 200 d after explosion. The first spectrum is characterised by a blue continuum with a blackbody temperature of ∼ 24, 000 K and flash-ionised emission lines. After about one week, the spectra of SN 2015bf evolve like those of a regular SN II. From the luminosity of the narrow emission component of Hα, we deduce that the mass-loss rate is larger than ∼ 3.7 × 10−3 M☉ yr−1. The disappearance of the flash features in the first week after explosion indicates that the circumstellar material is confined within ∼ 6 × 1014 cm. Thus, we suggest that the progenitor of SN 2015bf experienced violent mass loss shortly before the supernova explosion. The multiband light curves show that SN 2015bf has a high peak luminosity with an absolute visual magnitude MV = −18.11 ±0.08 mag and a fast post-peak decline with a V-band decay of 1.22 ±0.09 mag within ∼ 50 d after maximum light. Moreover, the R-band tail luminosity of SN 2015bf is fainter than that of SNe II with similar peak by 1–2 mag, suggesting a small amount of 56Ni (∼ 0.009 M☉) synthesised during the explosion. Such a low nickel mass indicates that the progenitor of SN 2015bf could be a super-asymptotic-giant-branch star that collapsed owing to electron capture. Copyright © 2021, The Authors. All rights reserved.

关键词： Supernovae

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