TYPE IIn SUPERNOVA SN 2010jl: OPTICAL OBSERVATIONS FOR OVER 500 DAYS AFTER EXPLOSION
文献类型：期刊论文
| 作者 | Zhang, Tianmeng1,2 ; Wang, Xiaofeng3,4; Wu, Chao1; Chen, Juncheng3,4; Chen, Jia3,4; Liu, Qin3,4; Huang, Fang3,4,5; Liang, Jide3,4; Zhao, Xulin3,4; Lin, Lin6
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| 刊名 | ASTRONOMICAL JOURNAL
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| 出版日期 | 2012-11-01 |
| 卷号 | 144期号:5 |
| 关键词 | supernovae: general supernovae: individual (SN 2010jl) |
| 英文摘要 | 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. |
| 收录类别 | SCI |
| 语种 | 英语 |
| WOS记录号 | WOS:000310530400007 |
| 源URL | [http://ir.bao.ac.cn/handle/114a11/6207]  |
| 专题 | 国家天文台_光学天文研究部 |
| 作者单位 | 1.Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China 2.Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ, Beijing 100012, 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.Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China 6.Univ Sci & Technol China, Ctr Astrophys, Hefei 230026, Anhui, Peoples R China 7.Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China 8.Inst Astrophys Paris, Paris, France 9.Univ Paris 06, F-75252 Paris 05, France 10.Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Peoples R China |
| 推荐引用方式 GB/T 7714 | Zhang, Tianmeng,Wang, Xiaofeng,Wu, Chao,et al. TYPE IIn SUPERNOVA SN 2010jl: OPTICAL OBSERVATIONS FOR OVER 500 DAYS AFTER EXPLOSION[J]. ASTRONOMICAL JOURNAL,2012,144(5). |
| APA | Zhang, Tianmeng.,Wang, Xiaofeng.,Wu, Chao.,Chen, Juncheng.,Chen, Jia.,...&Ma, Jun.(2012).TYPE IIn SUPERNOVA SN 2010jl: OPTICAL OBSERVATIONS FOR OVER 500 DAYS AFTER EXPLOSION.ASTRONOMICAL JOURNAL,144(5). |
| MLA | Zhang, Tianmeng,et al."TYPE IIn SUPERNOVA SN 2010jl: OPTICAL OBSERVATIONS FOR OVER 500 DAYS AFTER EXPLOSION".ASTRONOMICAL JOURNAL 144.5(2012). |
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来源：国家天文台
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