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arXiv 2020年

作者： Jiang, C. Cunha, M. Christensen-Dalsgaard, J. Zhang, Q.S. School of Physics and Astronomy Sun Yat-Sen University No. 135 Xingang Xi Road Guangzhou510275 China Instituto de Astrofísica e Ciências do Espaço Universidade do Porto CAUP Rua das Estrelas PortoPT4150-762 Portugal School of Physics and Astronomy University of Birmingham BirminghamB15 2TT United Kingdom Stellar Astrophysics Centre Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Yunnan Observatories 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 Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China University of Chinese Academy of Sciences Beijing100049 China

Thanks to the high quality data of space missions, the detection of mixed modes has become possible in numerous stars. In this work, we investigate how the mixing character of dipolar mixed modes changes with stellar evolution, as well as with frequency within each stellar model. This is achieved by monitoring the variations in the coupling strength and the period spacing of dipolar mixed modes in red-giant models. These parameters are measured by fitting the asymptotic expansion of mixed modes to the model frequencies of a grid of red-giant models with masses between 1.0 and 2.0 Mo and three different chemical abundances. The coupling strength and the period spacing decrease with stellar evolution. We find that the slopes of their decreasing trends depend on the radial order of the pressure mode component. A non-negligible increase of the coupling strength with frequency by up to around 40% is found in the observable frequency range for a set of red-giant models. On the contrary, no significant changes of the period spacing with frequency are found. The changes in the mixing character of the modes are in most cases affected by the model mass and metallicity. Buoyancy glitches also have an impact on the mixing character. Significant fluctuations in the estimated coupling strength and period spacing are found for models approaching the luminosity bump, if the glitch impact of the frequencies is not considered in the applied asymptotic expansion. Copyright © 2020, The Authors. All rights reserved.

关键词： Giant stars

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Erratum: Secondary-electron radiation accompanying hadronic GeV-TeV gamma-rays from supernova remnants

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Monthly Notices of the Royal Astronomical Society 2020年第4期494卷 5314-5314页

作者： Huang, Yan Li, Zhuo Wang, Wei Zhao, Xiaohong Department of Astronomy School of Physics Peking University Beijing 100871 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing 100871 China School of Physics and Technology Wuhan University Wuhan 430072 China Yunnan Observatories Chinese Academy of Sciences Kunming 650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing 100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650216 China

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Rates and delay times of Type Ia supernovae in the helium-enriched main-sequence donor scenario

arXiv

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arXiv 2018年

作者： Liu, Zheng-Wei Stancliffe, Richard J. Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Cas Kunming650216 China Center for Astronomical Mega-Science Cas Beijing100012 China Argelander-Institut für Astronomie Auf dem Hügel 71 BonnD-53121 Germany

The nature of the progenitors of Type Ia supernovae (SNe Ia) remains a mystery. Comparing theoretical rates and delay-time distributions of SNe Ia with those inferred observationally can constrain their progenitor models. In this work, taking thermohaline mixing into account in the helium-enriched main-sequence (HEMS) donor scenario, we address rates and delay times of SNe Ia in this channel by combining the results of self-consistent binary evolution calculations with population synthesis models. We find that the Galactic SN Ia rate from the HEMS donor scenario is around 0.6-1.2 × 10-3yr-1, which is about 30% of the observed rate. Delay times of SNe Ia in this scenario cover a wide range of 0.1-1.0Gyr. We also present the pre-explosion properties of companion stars in the HEMS donor scenario, which will be helpful for placing constraints on SN Ia progenitors through analyzing their pre-explosion images. Copyright © 2018, The Authors. All rights reserved.

关键词： Helium

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BinCodex: a common output format for binary population synthesis

arXiv

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arXiv 2023年

作者： Valli, Ruggero Graziani, Luca Agrawal, Poojan Arca Sedda, Manuel Artale, M. Celeste Bobrick, Alexey Breivik, Katelyn Chakraborty, Srija Çalşskan, Mesut Chen, Xuefei Eldridge, Jan J. Escobar, Gastón J. Gossage, Seth Han, Zhanwen Iorio, Giuliano Korb, Erika Korol, Valeriya Kruckow, Matthias U. Larson, Shane L. Laurentiu, Caramete Li, Zhenwei Mandel, Ilya Menu, Jonathan Nelemans, Gijs Rodriguez-Segovia, Nicolas Ruiter, Ashley J. Tang, Petra Toonen, Silvia Sgalletta, Cecilia Strokov, Vladimir Sun, Meng Willcox, Reinhold Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Straße 1 Garching85741 Germany Dipartimento di Fisica Sapienza Università di Roma Piazzale Aldo Moro 5 Roma00185 Italy Department of Physics and Astronomy The University of North Carolina at Chapel Hill Chapel HillNC27599 United States Gran Sasso Science Institute V.le F. Crispi L'Aquila67100 Italy L'Aquila67100 Italy INAF Osservatorio Astronomico d'Abruzzo Via M. Maggini snc Teramo64100 Italy Instituto de Astrofísica Facultad de Ciencias Exactas Universidad Andres Bello Fernandez Concha 700 Santiago Chile Physics Department Technion - Israel Institute of Technology Haifa3200002 Israel Department of Physics McWilliams Center for Cosmology Carnegie Mellon University 5000 Forbes Avenue PittsburghPA15213 United States Department of Physics Scuola Normale Superiore Piazza dei Cavalieri 7 PI Pisa56126 Italy Department of Physics & Astronomy Johns Hopkins University 3400 North Charles Street BaltimoreMD21218 United States Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Science China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China Department of Physics University of Auckland Private Bag 92019 Auckland New Zealand Dipartimento di Fisica e Astronomia Università di Padova Vicolo dell'Osservatorio 3 Padova35122 Italy Northwestern University 1800 Sherman Ave EvanstonIL60201 United States Département d'Astronomie Université de Genève Chemin Pegasi 51 VersoixCH-1290 Switzerland Université de Genève GenevaCH-1211 Switzerland Center for Interdisciplinary Exploration & Research in Astrophysics Department of Physics & Astronomy Northwestern University EvanstonIL60201 United States Cosmology and Astroparticle Physics Laboratory Institute of Space Science Atomistilor Street 409 Magurele077125 Romania School of Physics and Astronomy Monash Uni

This document describes BinCodex, a common format for the output of binary population synthesis (BPS) codes agreed upon by the members of the LISA Synthetic UCB Catalogue Group. The goal of the format is to provide a common reference framework to describe the evolution of a single, isolated binary system or a population of isolated binaries. © 2023, CC BY.

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Optical and Near-infrared Observations of SN 2023ixf for over 600 days after the Explosion

arXiv

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arXiv 2025年

作者： Li, Gaici Wang, Xiaofeng Yang, Yi Pastorello, A. Reguitti, A. Valerin, G. Ochner, P. Cai, Yongzhi Iijima, T. Munari, U. Salmaso, I. Farina, A. Cazzola, R. Trabacchin, N. Fiscale, S. Ciroi, S. Mura, A. Siviero, A. Cabras, F. Pabst, M. Taubenberger, S. Vogl, C. Fiorin, C. Liu, Jialian Chen, Liyang Xiang, Danfeng Mo, Jun Li, Liping Wang, Zhenyu Zhang, Jujia Zhai, Qian Mirzaqulov, D.O. Ehgamberdiev, S.A. Filippenko, Alexei V. Yan, Shengyu Hu, Maokai Ma, Xiaoran Xia, Qiqi Gao, Xing Li, Wenxiong Department of Physics Tsinghua University Beijing100084 China Department of Astronomy University of California BerkeleyCA94720-3411 United States INAF - Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 Padova35122 Italy INAF - Osservatorio Astronomico di Brera Via E. Bianchi 46 LC Merate23807 Italy Dipartimento di Fisica e Astronomia Università Degli Studi di Padova PD Padova35121 Italy Yunnan Observatories Chinese Academy of Sciences Kunming650216 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China INAF-Osservatorio Astronomico di Capodimonte Salita Moiariello 16 Napoli80131 Italy CISAS G. Colombo University of Padova via Venezia 15 Padova35131 Italy UNESCO Chair"Environment Resources and Sustainable Development" Department of Science and Technology Parthenope University of Naples Italy INAF Osservatorio Astronomico di Capodimonte Salita Moiariello 16 NaplesI-80131 Italy Max-Planck-Institut fur Astrophysik Karl-Schwarzschild Straße 1 Garching85748 Germany Beijing Planetarium Beijing Academy of Sciences and Technology Beijing100044 China University of Chinese Academy of Sciences Beijing100049 China Ulugh Beg Astronomical Institute Astronomy Street 33 Tashkent100052 Uzbekistan National University of Uzbekistan Tashkent100174 Uzbekistan School of Space Science and Technology Shandong University Shandong Weihai264209 China Xingming Observatory Urumqi830000 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China

Context. We present a comprehensive photometric and spectroscopic study of the nearby Type II supernova (SN) 2023ixf, with our extensive observations spanning the phases from ∼3 to over 600 days after the first light. Aims. The aim of this study is to obtain key information on the explosion properties of SN 2023ixf and the nature of its progenitor. Methods. The observational properties of SN 2023ixf are compared with those of a representative sample of Type IIP/IIL SNe to investigate commonalities and diversities. We conduct a detailed analysis of temporal evolution of major spectral features observed throughout different phases of the SN 2023ixf explosion. Several key interpretations are addressed through a comparison between the data and the model spectra predicted by non-local thermodynamic equilibrium (non-LTE) radiative-transfer calculations for progenitor stars within a range of zero-age main sequence (ZAMS) masses. Results. Our observations indicate that SN 2023ixf is a transitional SN that bridges the gap between Type IIP and IIL subclasses of H-rich SNe, characterized by a relatively short plateau ( 70 d) in the light curve. It shows a rather prompt spectroscopic evolution toward the nebular phase;emission lines of Na, O, H, and Ca in nebular spectra all exhibit multipeak profiles, which might be attributed to bipolar distribution of the ejecta. In particular, the Hα profile can be separated into two central peaked components (with a velocity of about 1500 km s−1) that is likely due to nickel-powered ejecta and two outer peak/box components (with a velocity extending up to ∼ 8000 km s−1) that can arise from interaction of the outermost ejecta with a circumstellar shell at a distance of ∼ 6.2 × 1015 cm. The nebular-phase spectra of SN 2023ixf show good agreement with those predicted by a non-LTE radiative-transfer code for progenitor stars with a ZAMS mass ranging from 15 to 19 M☉. A distance D = 6.35+−00.3139 Mpc is estimated for M101 based on the expanding

关键词： Supernovae

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Why are peculiar type ia supernovae more likely to show the signature of a single-degenerate model?

arXiv

引用

arXiv 2018年

作者： Meng, Xiang-Cun Han, Zhan-Wen 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

Although type Ia supernovae (SNe Ia) are very useful in many astrophysical fields, their exact progenitor nature is still unclear. A basic method to distinguish the different progenitor models is to search the signal from the single-degenerate (SD) model, e.g., the signal for the existence of a nondegenerate companion before or after supernova explosion. Observationally, some SNe Ia show such signals, while the others do not. Here, we propose a universal model to explain these observations based on the spin-up/spin-down model, in which a white dwarf (WD) will experience a spin-down phase before supernova explosion, and the spin-down timescale is determined by its initial mass, i.e., the more massive the initial WD, the shorter the spin-down timescale and then the more likely the SN Ia is to show the SD signature. Therefore, our model predicts that the SNe Ia from hybrid carbon-oxygen-neon WDs are more likely to show the SD signature observationally, as some peculiar SNe Ia showed. Copyright © 2018, The Authors. All rights reserved.

关键词： White dwarfs

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Still brighter than pre-explosion, SN 2012Z did not disappear: Comparing hubble space telescope observations a decade apart

arXiv

引用

arXiv 2021年

作者： Mccully, Curtis Jha, Saurabh W. Scalzo, Richard A. Howell, D. Andrew Foley, Ryan J. Zeng, Yaotian Liu, Zheng-Wei Hosseinzadeh, Griffin Bildsten, Lars Riess, Adam G. Kirshner, Robert P. Marion, G.H. Camacho-Neves, Yssavo Las Cumbres Observatory 6740 Cortona Dr Ste 102 GoletaCA93117-5575 United States Department of Physics University of California Santa BarbaraCA93106-9530 United States Department of Physics and Astronomy Rutgers The State University of New Jersey 136 Frelinghuysen Road PiscatawayNJ08854 United States School of Mathematics and Statistics The University of Sydney CamperdownNSW2006 Australia Centre for Translational Data Science University of Sydney DarlingtonNSW2008 Australia Department of Astronomy and Astrophysics University of California Santa CruzCA92064 United States Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650216 China University of Chinese Academy of Science Beijing100012 China Center for Astronomical Mega-Science CAS Beijing100012 China Center for Astrophysics - Harvard and Smithsonian 60 Garden Street CambridgeMA02138-1516 United States Kavli Institute for Theoretical Physics University of California Santa BarbaraCA93106 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Department of Physics and Astronomy Johns Hopkins University BaltimoreMD21218 United States Gordon and Betty Moore Foundation 1661 Page Mill Road Palo AltoCA94304 United States University of Texas at Austin 1 University Station C1400 AustinTX78712-0259 United States

Type Iax supernovae represent the largest class of peculiar white-dwarf supernovae. The type Iax SN 2012Z in NGC 1309 is the only white dwarf supernova with a detected progenitor system in pre-explosion observations. Deep Hubble Space Telescope images taken before SN 2012Z show a luminous, blue source that we have interpreted as a helium-star companion (donor) to the exploding white dwarf. We present here late-time HST observations taken ∼1400 days after the explosion to test this model. We find the SN light curve can empirically be fit by an exponential decay model in magnitude units. The fitted asymptotic brightness is within 10% of our latest measurements and approximately twice the brightness of the pre-explosion source. The decline of the light curve is too slow to be powered by 56Co or 57Co decay: if radioactive decay is the dominate power source, it must be from longer half-life species like 55Fe. Interaction with circumstellar material may contribute to the light curve, as may shock heating of the companion star. Companion-star models underpredict the observed flux in the optical, producing most of their flux in the UV at these epochs. A radioactively-heated bound remnant, left after only a partial disruption of the white dwarf, is also capable of producing the observed excess late-time flux. Our analysis suggests that the total ejecta + remnant mass is consistent with the Chandrasekhar mass for a range of type Iax supernovae. Copyright © 2021, The Authors. All rights reserved.

关键词： Supernovae

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The single-degenerate model for the progenitors of accretion-induced collapse events

arXiv

引用

arXiv 2018年

作者： Wang, Bo 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 Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China

It has been suggested that the accretion-induced collapse (AIC) of an oxygen-neon white dwarf (ONe WD) to a neutron star is a theoretically predicted outcome in stellar evolution, likely relating to the formation of some neutron star systems. However, the progenitor models of AIC events are still not well studied, and recent studies indicated that CO WD+He star systems may also contribute to the formation of neutron star systems through AIC process when off-centre carbon ignition happens on the surface of the CO WD. In this work, I studied the single-degenerate (SD) model of AIC events in a systematic way, including the contribution of the CO WD+He star channel and the ONe WD+MS/RG/He star channels. Firstly, I gave the initial parameter space of these SD channels for producing AIC events in the orbital period–secondary mass plane based on detailed binary evolution computations. Then, according to a binary population synthesis approach, I gave the rates and delay times of AIC events for these SD channels based on their initial parameter space. I found that the rates of AIC events in our galaxy are in the range of ∼ 0.3 − 0.9 × 10−3 yr−1, and that their delay times are >30 Myr. I also found that the ONe WD+He star channel is the main way to produce AIC events, and that the CO WD+He star channel cannot be ignored when studying the progenitors of AIC events. Copyright © 2018, The Authors. All rights reserved.

关键词： White dwarfs

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Sn 2018hti: A nearby superluminous supernova discovered in a metal-poor galaxy

arXiv

引用

arXiv 2020年

作者： Lin, W.L. Wang, X.F. Li, W.X. Zhang, J.J. Mo, J. Sai, H.N. Zhang, X.H. Filippenko, A.V. Zheng, W.K. Brink, T.G. Baron, E. DerKacy, J.M. Ehgamberdiev, S.A. Mirzaqulov, D. Li, X. Zhang, J.C. Yan, S.Y. Xi, G.B. Hsiao, Y. Zhang, T.M. Wang, L.J. Liu, L.D. Xiang, D.F. Wu, C.Y. Rui, L.M. Chen, Z.H. Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 China 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 Department of Astronomy University of California BerkeleyCA94720-3411 United States Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Homer L. Dodge Department of Physics and Astronomy University of Oklahoma NormanOK73019 United States Ulugh Beg Astronomical Institute Uzbekistan Academy of Sciences Uzbekistan Tashkent100052 Uzbekistan Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing10101 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Astroparticle Physics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China Department of Astronomy Beijing Normal University Beijing100875 China

SN 2018hti is a Type I superluminous supernova (SLSN I) with an absolute g-band magnitude of −22.2 at maximum brightness, discovered in a metal-poor galaxy at a redshift of 0.0612. We present extensive photometric and spectroscopic observations of this supernova, covering the phases from ∼ −35 days to more than +340 days from the r-band maximum. Combining our BVgri-band photometry with Swift UVOT optical/ultraviolet photometry, we calculated the peak luminosity as ∼ 3.5 × 1044 erg s−1. Modeling the observed light curve reveals that the luminosity evolution of SN 2018hti can be produced by an ejecta mass of 5.8 M and a magnetar with a magnetic field of B = 1.8 × 1013 G having an initial spin period of P0 = 1.8 ms. Based on such a magnetar-powered scenario and a larger sample, a correlation between the spin of the magnetar and the kinetic energy of the ejecta can be inferred for most SLSNe I, suggesting a self-consistent scenario. Like for other SLSNe I, the host galaxy of SN 2018hti is found to be relatively faint (Mg = −17.75 mag) and of low metallicity (Z = 0.3 Z ), with a star-formation rate of 0.3 M yr−1. According to simulation results of single-star evolution, SN 2018hti could originate from a massive, metal-poor star with a zero-age main sequence (ZAMS) mass of 25–40 M , or from a less massive rotating star with MZAMS ≈ 16–25 M . For the case of a binary system, its progenitor could also be a star with MZAMS & 25 M . Copyright © 2020, The Authors. All rights reserved.

关键词： Luminance

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Properties of Radial Velocities measurement based on LAMOST-II Medium-Resolution Spectroscopic Observations

arXiv

引用

arXiv 2019年

作者： Wang, R. Luo, A.-L. Chen, J.-J. Bai, Z.-R. Chen, L. Chen, X.-F. Dong, S.-B. Du, B. Fu, J.-N. Han, Z.-W. Hou, J.-L. Hou, Y.-H. Hou, W. Jiang, D.-K. Kong, X. Li, L.-F. Liu, C. Liu, J.-M. Qin, L. Shi, J.-R. Tian, H. Wu, H. Wu, C.-J. Xie, J.-W. Zhang, H.-T. Zhang, S. Zhao, G. Zhao, Y.-H. Zhong, J. Zong, W.-K. Zuo, F. Wu, H. Wu, C.-J. Xie, J.-W. Zhang, H.-T. Zhang, S. Zhao, G. Zhao, Y.-H. Zhong, J. Zong, W.-K. Zuo, F. Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Department of Astronomy Beijing Normal University Beijing100875 China Nanjing Institute of Astronomical Optics and Technology National Astronomical Observatories Chinese Academy of Sciences Nanjing210042 China School of Astronomy and Space Science Nanjing University Nanjing210093 China Key Laboratory of Modern Astronomy and Astrophysics in Ministry of Education Nanjing University Nanjing210093 China

The radial velocity (RV) is a basic physical quantity which can be determined through Doppler shift of the spectrum of a star. The precision of RV measurement depends on the resolution of the spectrum we used and the accuracy of wavelength calibration. In this work, radial velocities of LAMOST-II medium resolution (R ∼ 7500) spectra are measured for 1,594,956 spectra (each spectrum has two wavebands) through matching with templates. A set of RV standard stars are used to recalibrate the zero point of the measurement, and some reference sets with RVs derived from medium/high-resolution observations are used to evaluate the accuracy of the measurement. Comparing with reference sets, the accuracy of our measurement can get 0.0227 km1 s-1with respect to radial velocities standard stars. The intrinsic precision is estimated with the multiple observations of single stars, which can achieve to 1.36 km s-1,1.08 km s-1, 0.91 km s-1for the spectra at signal-to-noise levels of 10, 20, 50, respectively. Copyright © 2019, The Authors. All rights reserved.

关键词： Stars

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