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TYPE IIn SUPERNOVA SN 2010jl: OPTICAL OBSERVATIONS FOR OVER 500 DAYS AFTER EXPLOSION
Zhang, TM1,2; Wang, XF3; Wu, C1; Chen, JC3; Chen, J3; Liu, Q3; Huang, F3,4; Liang, JD3; Zhao, XL3; Lin, L5; Wang, M6; Dennefeld, M7; Zhang JJ(张居甲)8; Zhai, M1,2; Wu, H1,2; Fan, Z1,2; Zou, H1,2; Zhou, X1,2; Ma, J1,2; Zhang, TM (reprint author), Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China.
发表期刊ASTRONOMICAL JOURNAL
2012-11
卷号144期号:5
DOI10.1088/0004-6256/144/5/131
产权排序第8完成单位
收录类别SCI
关键词Supernovae: General Supernovae: Individual (Sn 2010jl)
摘要We present extensive optical observations of a Type IIn supernova (SN IIn) 2010jl for the first 1.5 years after its discovery. The UBVRI light curves demonstrated an interesting two-stage evolution during the nebular phase, which almost flatten out after about 90 days from the optical maximum. SN 2010jl has one of the highest intrinsic Ha luminosities ever recorded for an SN IIn, especially at late phase, suggesting a strong interaction of SN ejecta with the dense circumstellar material (CSM) ejected by the progenitor. This is also indicated by the remarkably strong Balmer lines persisting in the optical spectra. One interesting spectral evolution about SN 2010jl is the appearance of asymmetry of the Balmer lines. These lines can be well decomposed into a narrow component and an intermediate-width component. The intermediate-width component showed a steady increase in both strength and blueshift with time until t similar to 400 days after maximum, but it became less blueshifted at t similar to 500 days, when the line profile appeared relatively symmetric again. Owing to the fact that a pure reddening effect will lead to a sudden decline of the light curves and a progressive blueshift of the spectral lines, we therefore propose that the asymmetric profiles of H lines seen in SN 2010jl are unlikely due to the extinction by newly formed dust inside the ejecta, contrary to the explanation by some early studies. Based on a simple CSM-interaction model, we speculate that the progenitor of SN 2010jl may suffer a gigantic mass loss (similar to 30-50 M-circle dot) a few decades before explosion. Considering a slow-moving stellar wind (e. g., similar to 28 km s(-1)) inferred for the preexisting, dense CSM shell and the extremely high mass-loss rate (1-2 M-circle dot yr(-1)), we suggest that the progenitor of SN 2010jl might have experienced a red supergiant stage and may explode finally as a post-red supergiant star with an initial mass above 30-40 M-circle dot.
项目资助者Young Researcher Grant of National Astronomical Observatories, Chinese Academy of Sciences ; National Natural Science Foundation of China (NSFC) [11073013, 11178003] ; Foundation of Tsinghua University [2011Z02170] ; Major State Basic Research Development Program [2009CB824800] ; NSFC [10903010, 11003021, 11073032]
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0004-6256
URL查看原文
WOS记录号WOS:000310530400007
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]LUMINOUS BLUE VARIABLES ; CORE-COLLAPSE SUPERNOVAE ; DUST FORMATION ; MASSIVE STARS ; X-RAY ; PROGENITOR ; PHOTOMETRY ; EVOLUTION ; SPECTROSCOPY ; IINSN1998S
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/5416
专题丽江天文观测站(南方基地)
通讯作者Zhang, TM (reprint author), Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China.
作者单位1.National Astronomical Observatories of China, Chinese Academy of Sciences, Beijing 100012, People's Republic of China
2.Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People's Republic of China
3.Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing 100084, China
4.Department of Astronomy, Beijing Normal University, Beijing, 100875, People's Republic of China
5.Center for Astrophysics, University of Science and Technology of China, No. 96, JinZhai Road Baohe District, Hefei, Anhui 230026, People's Republic of China
6.Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, 210008, People's Republic of China
7.Institut d'Astrophysique de Paris, and University Pierre et Marie Curie (Paris 6), France
8.Yunnan Astronomical Observatory, Chinese Academy of Sciences, Kunming 650011, People's Republic of China
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Zhang, TM,Wang, XF,Wu, C,et al. TYPE IIn SUPERNOVA SN 2010jl: OPTICAL OBSERVATIONS FOR OVER 500 DAYS AFTER EXPLOSION[J]. ASTRONOMICAL JOURNAL,2012,144(5).
APA Zhang, TM.,Wang, XF.,Wu, C.,Chen, JC.,Chen, J.,...&Zhang, TM .(2012).TYPE IIn SUPERNOVA SN 2010jl: OPTICAL OBSERVATIONS FOR OVER 500 DAYS AFTER EXPLOSION.ASTRONOMICAL JOURNAL,144(5).
MLA Zhang, TM,et al."TYPE IIn SUPERNOVA SN 2010jl: OPTICAL OBSERVATIONS FOR OVER 500 DAYS AFTER EXPLOSION".ASTRONOMICAL JOURNAL 144.5(2012).
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