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A LUMINOUS PECULIAR TYPE IA SUPERNOVA SN 2011HR: MORE LIKE SN 1991T OR SN 2007if?
Zhang JJ(张居甲)1,2,3; Wang, Xiao-Feng3; Sasdelli, Michele4,5; Zhang, Tian-Meng6; Liu, Zheng-Wei7; Mazzali, Paolo A.4,5; Meng XC(孟祥存)1,2; Maeda, Keiichi8,9; Chen, Jun-Cheng3; Huang, Fang3; Zhao, Xu-Lin3; Zhang, Kai-Cheng3; Zhai Q(翟倩)1,2,10; Pian, Elena11,12; Wang B(王博)1,2; Chang L(常亮)1,2; Yi WM(易卫敏)1,2; Wang CJ(王传军)1,2,10; Wang XL(王雪利)1,2; Xin YX(辛玉新)1,2; Wang JG(王建国)1,2; Lun BL(伦宝利)1,2; Zheng XM(郑向明)1,2; Zhang XL(张西亮)1,2; Fan YF(范玉峰)1,2; Bai JM(白金明)1,2
发表期刊ASTROPHYSICAL JOURNAL
2016-02-01
卷号817期号:2
DOI10.3847/0004-637X/817/2/114
产权排序第1完成单位
收录类别SCI
关键词Galaxies: Individual (Ngc 2691) Supernovae: General Supernovae: Individual (Sn 2011hr Sn 1991t Sn 2007if)
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.
项目资助者Chinese Academy of Sciences (CAS) ; People's Government of Yunnan Province ; National Science Foundation of China (NSFC) (11403096, 11178003, 11325313, 11133006, 11361140347, 11203034, 11473063, 11322327, 11103072, 11203078, 11303085, 11203070, 11103078) ; Major State Basic Research Development Program(2013CB834903) ; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the CAS(XDB09000000) ; Key Research Program of the CAS(KJZD-EW-M06) ; Western Light Youth Project ; Youth Innovation Promotion Association of the CAS ; Open Project Program of the Key Laboratory of Optical Astronomy, NAOC, CAS ; key Laboratory for Research in Galaxies and Cosmology of the CAS
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0004-637X
URL查看原文
归档日期2016-03-28
WOS记录号WOS:000369437900031
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]GRAVITATIONALLY CONFINED DETONATION ; NEAR-INFRARED OBSERVATIONS ; HIGH-VELOCITY FEATURES ; HUBBLE-SPACE-TELESCOPE ; LIGHT CURVES ; ABUNDANCE STRATIFICATION ; WHITE-DWARF ; SPECTROSCOPIC OBSERVATIONS ; ULTRAVIOLET OBSERVATIONS ; EXPLOSION
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/9337
专题丽江天文观测站(南方基地)
中国科学院天体结构与演化重点实验室
作者单位1.Yunnan Observatories (YNAO), Chinese Academy of Sciences, Kunming 650011, China
2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, China
3.Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, China
4.Astrophysics Research Institute, Liverpool John Moores University, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK
5.Max-Planck Institute fur Astrophysics, D-85748 Garching, Germany
6.National Astronomical Observatories of China (NAOC), Chinese Academy of Sciences, Beijing 100012, China
7.Argelander-Institut für Astronomie, Auf dem Hügel 71, D-53121, Bonn, Germany
8.Department of Astronomy, Kyoto University, Kyoto, 606-8502, Japan
9.Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan
10.University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China
11.INAF-IASF-Bo, via Gobetti, 101, I-40129 Bologna, Italy
12.Scuola Normale Superiore, Piazza dei Cavalieri 7, I-56126 Pisa, Italy
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Zhang JJ,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 JJ.,Wang, Xiao-Feng.,Sasdelli, Michele.,Zhang, Tian-Meng.,Liu, Zheng-Wei.,...&Bai JM.(2016).A LUMINOUS PECULIAR TYPE IA SUPERNOVA SN 2011HR: MORE LIKE SN 1991T OR SN 2007if?.ASTROPHYSICAL JOURNAL,817(2).
MLA Zhang JJ,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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