ASASSN-14ms: The Most Energetic Known Explosion of a Type Ibn Supernova and Its Physical Origin | |
Wang, Xiaofeng12,13; Lin, Weili13; Zhang JJ(张居甲)10,11; Zhang, Tianmeng8,9; Cai, Yongzhi13; Zhang, Kaicheng13; Filippenko, Alexei V.6,7; Graham, Melissa5; Maeda, Keiichi4; Mo, Jun13 | |
刊名 | ASTROPHYSICAL JOURNAL |
2021-08 | |
卷号 | 917期号:2 |
ISSN号 | 0004-637X |
DOI | 10.3847/1538-4357/ac0c17 |
产权排序 | 第3完成单位 |
文献子类 | Article |
英文摘要 | ASASSN-14ms may represent the most luminous Type Ibn supernova (SN Ibn) ever detected, with an absolute U-band magnitude brighter than -22.0 mag and a total bolometric luminosity >1.0 x 10(44) erg s(-1) near maximum light. The early-time spectra of this SN are characterized by a blue continuum on which are superimposed narrow P Cygni profile lines of He i, suggesting the presence of slowly moving (similar to 1000 km s(-1)), He-rich circumstellar material (CSM). At 1-2 months after maximum brightness, the He i line profiles become only slightly broader, with blueshifted velocities of 2000-3000 km s(-1), consistent with the CSM shell being continuously accelerated by the SN light and ejecta. Like most SNe Ibn, the light curves of ASASSN-14ms show rapid post-peak evolution, dropping by similar to 7 mag in the V band over three months. Such a rapid post-peak decline and high luminosity can be explained by interaction between SN ejecta and helium-rich CSM of 0.9 M (circle dot) at a distance of similar to 10(15) cm. The CSM around ASASSN-14ms is estimated to originate from a pre-explosion event with a mass-loss rate of 6.7 M (circle dot) yr(-1) (assuming a velocity of similar to 1000 km s(-1)), which is consistent with abundant He-rich material violently ejected during the late Wolf-Rayet (WN9-11 or Opfe) stage. After examining the light curves for a sample of SNe Ibn, we find that the more luminous ones tend to have slower post-peak decline rates, reflecting that the observed differences may arise primarily from discrepancies in the CSM distribution around the massive progenitors. |
学科主题 | 天文学 ; 恒星与银河系 |
URL标识 | 查看原文 |
出版地 | TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND |
资助项目 | National Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[12033003] ; National Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11633002] ; Major State Basic Research Development ProgramNational Basic Research Program of China[2016YFA0400803] ; Scholar Program of Beijing Academy of Science and Technology[DZ:BS202002] ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; TABASGO Foundation ; Christopher R. Redlich Fund ; U.C. Berkeley Miller Institute for Basic Research in Science ; Japan Society for the Promotion of Science (JSPS) KAKENHI grantMinistry of Education, Culture, Sports, Science and Technology, Japan (MEXT)Japan Society for the Promotion of ScienceGrants-in-Aid for Scientific Research (KAKENHI)[JP18H05223] ; Japan Society for the Promotion of Science (JSPS) KAKENHI grantMinistry of Education, Culture, Sports, Science and Technology, Japan (MEXT)Japan Society for the Promotion of ScienceGrants-in-Aid for Scientific Research (KAKENHI)[JP20H00174] ; Japan Society for the Promotion of Science (JSPS) KAKENHI grantMinistry of Education, Culture, Sports, Science and Technology, Japan (MEXT)Japan Society for the Promotion of ScienceGrants-in-Aid for Scientific Research (KAKENHI)[JP20H04737] ; Chinese Academy of SciencesChinese Academy of Sciences ; People's Government of Yunnan Province ; W. M. Keck FoundationW.M. Keck Foundation |
WOS关键词 | RICH CIRCUMSTELLAR MEDIUM ; WOLF-RAYET STAR ; MASSIVE STARS ; CORE-COLLAPSE ; LIGHT CURVES ; OPTICAL OBSERVATIONS ; SN 2009JF ; EVOLUTION ; TRANSIENT ; EMISSION |
WOS研究方向 | Astronomy & Astrophysics |
语种 | 英语 |
出版者 | IOP PUBLISHING LTD |
WOS记录号 | WOS:000687842200001 |
资助机构 | National Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[12033003, 11633002] ; Major State Basic Research Development ProgramNational Basic Research Program of China[2016YFA0400803] ; Scholar Program of Beijing Academy of Science and Technology[DZ:BS202002] ; Open Project Program of the Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences ; TABASGO Foundation ; Christopher R. Redlich Fund ; U.C. Berkeley Miller Institute for Basic Research in Science ; Japan Society for the Promotion of Science (JSPS) KAKENHI grantMinistry of Education, Culture, Sports, Science and Technology, Japan (MEXT)Japan Society for the Promotion of ScienceGrants-in-Aid for Scientific Research (KAKENHI)[JP18H05223, JP20H00174, JP20H04737] ; Chinese Academy of SciencesChinese Academy of Sciences ; People's Government of Yunnan Province ; W. M. Keck FoundationW.M. Keck Foundation |
内容类型 | 期刊论文 |
版本 | 出版稿 |
源URL | [http://ir.ynao.ac.cn/handle/114a53/24524] |
专题 | 云南天文台_丽江天文观测站(南方基地) |
通讯作者 | Wang, Xiaofeng |
作者单位 | 1.Department of Physical Science, Hiroshima University, Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan 2.Astroparticle Physics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, People's Republic of China; 3.Physics and Astronomy Department, Texas A&M University, College Station, TX 77843, USA; 4.Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan; 5.Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580, USA; 6.Miller Institute for Basic Research in Science, University of California, Berkeley, CA 94720, USA; 7.Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA; 8.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 101408, People's Republic of China; 9.Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People's Republic of China; 10.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, People's Republic of China; |
推荐引用方式 GB/T 7714 | Wang, Xiaofeng,Lin, Weili,Zhang JJ,et al. ASASSN-14ms: The Most Energetic Known Explosion of a Type Ibn Supernova and Its Physical Origin[J]. ASTROPHYSICAL JOURNAL,2021,917(2). |
APA | Wang, Xiaofeng.,Lin, Weili.,Zhang JJ.,Zhang, Tianmeng.,Cai, Yongzhi.,...&Zhai Q.(2021).ASASSN-14ms: The Most Energetic Known Explosion of a Type Ibn Supernova and Its Physical Origin.ASTROPHYSICAL JOURNAL,917(2). |
MLA | Wang, Xiaofeng,et al."ASASSN-14ms: The Most Energetic Known Explosion of a Type Ibn Supernova and Its Physical Origin".ASTROPHYSICAL JOURNAL 917.2(2021). |
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