A LUMINOUS PECULIAR TYPE IA SUPERNOVA SN 2011HR: MORE LIKE SN 1991T OR SN 2007if?
文献类型：期刊论文
| 作者 | Zhang, Ju-Jia1,2,3,4; Wang, Xiao-Feng3,4; Sasdelli, Michele5,6; Zhang, Tian-Meng7 ; Liu, Zheng-Wei8; Mazzali, Paolo A.5,6; Meng, Xiang-Cun1,2; Maeda, Keiichi9,10; Chen, Jun-Cheng3,4; Huang, Fang3,4
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| 刊名 | ASTROPHYSICAL JOURNAL
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| 出版日期 | 2016-02-01 |
| 卷号 | 817期号:2 |
| 关键词 | galaxies: individual (NGC 2691) supernovae: general supernovae: individual (SN 2011hr, SN 1991T, SN 2007if) |
| 英文摘要 | Photometric and spectroscopic observations of a slowly declining, luminous Type Ia supernova (SN Ia) SN 2011hr in the starburst galaxy NGC 2691 are presented. SN. 2011hr is found to peak at MB = -19.84 +/- 0.40 mag, with a postmaximum decline rate Delta(m15)(B) = 0.92. +/- 0.03 mag. From the maximum-light bolometric luminosity, L = (2.30 +/- 0.90) x 10(43) erg s(-1), we estimate the mass of synthesized Ni-56 in SN 2011hr to be M(Ni-56) = 1.11 +/- 0.43M(circle dot). SN 2011hr appears more luminous than SN 1991T at around maximum light, and the absorption features from its intermediate-mass elements (IMEs) are noticeably weaker than those of the latter at similar phases. Spectral modeling suggests that SN 2011hr has IMEs of similar to 0.07 M-circle dot in the outer ejecta, which is much lower than the typical value of normal SNe Ia (i.e., 0.3-0.4 M-circle dot) and is also lower than the value of SN 1991T (i.e., similar to 0.18 M-circle dot). These results indicate that SN. 2011hr may arise from a Chandrasekhar-mass white dwarf progenitor that experienced a more efficient burning process in the explosion. Nevertheless, it is still possible that SN. 2011hr may serve as a transitional object connecting the SN 1991T-like SNe Ia with a superluminous subclass like SN 2007if given that the latter also shows very weak IMEs at all phases. |
| 收录类别 | SCI |
| 语种 | 英语 |
| WOS记录号 | WOS:000369437900031 |
| 源URL | [http://ir.bao.ac.cn/handle/114a11/5432]  |
| 专题 | 国家天文台_光学天文研究部 |
| 作者单位 | 1.Chinese Acad Sci, Yunnan Observ YNAO, Kunming 650011, Peoples R China 2.Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650011, Peoples R China 3.Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China 4.Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China 5.Liverpool John Moores Univ, Astrophys Res Inst, Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England 6.Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany 7.Chinese Acad Sci, NAOC, Beijing 100012, Peoples R China 8.Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany 9.Kyoto Univ, Dept Astron, Kyoto 6068502, Japan 10.Univ Tokyo, Kavli Inst Phys & Math Universe WPI, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan |
| 推荐引用方式 GB/T 7714 | Zhang, Ju-Jia,Wang, Xiao-Feng,Sasdelli, Michele,et al. A LUMINOUS PECULIAR TYPE IA SUPERNOVA SN 2011HR: MORE LIKE SN 1991T OR SN 2007if?[J]. ASTROPHYSICAL JOURNAL,2016,817(2). |
| APA | Zhang, Ju-Jia.,Wang, Xiao-Feng.,Sasdelli, Michele.,Zhang, Tian-Meng.,Liu, Zheng-Wei.,...&Bai, Jin-Ming.(2016).A LUMINOUS PECULIAR TYPE IA SUPERNOVA SN 2011HR: MORE LIKE SN 1991T OR SN 2007if?.ASTROPHYSICAL JOURNAL,817(2). |
| MLA | Zhang, Ju-Jia,et al."A LUMINOUS PECULIAR TYPE IA SUPERNOVA SN 2011HR: MORE LIKE SN 1991T OR SN 2007if?".ASTROPHYSICAL JOURNAL 817.2(2016). |
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来源：国家天文台
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