Type IIn Supernova SN 2010jl: Optical Observations for Over 500 Days After Explosion

Дата и время публикации : 2012-08-30T04:39:30Z

Авторы публикации и институты :
Tianmeng Zhang
Xiaofeng Wang
Chao Wu
Juncheng Chen
Jia Chen
Qin Liu
Fang Huang
Jide Liang
Xulin Zhao
Lin Li
Min Wang
Michel Dennefeld
Jujia Zhang
Meng Zhai
Hong Wu
Zhou Fan
Hu Zou
Xu Zhou
Jun Ma

Ссылка на журнал-издание: Ссылка на журнал-издание не найдена
Коментарии к cтатье: 34 pages, 9 figures, accepted for publication in AJ
Первичная категория: astro-ph.SR

Все категории : astro-ph.SR

Краткий обзор статьи: We present extensive optical observations of a Type IIn supernova (SN) 2010jl for the first 1.5 years after the 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 H_alpha luminosity ever recorded for a 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 ~ 400 days after maximum, but it became less blueshifted at t ~ 500 days when the line profile appeared relatively symmetric again. Owing to 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 is 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 (~ 30-50 M_sun) in a few decades before explosion. Considering a slow moving stellar wind (e.g., ~ 28 km/s) inferred for the preexisting, dense CSM shell and the extremely high mass-loss rate (1-2 M_sun per yr), we suggest that the progenitor of SN 2010jl might have experienced a red supergiant stage and explode finally as a post-red supergiant star with an initial mass above 30-40 M_sun.

Category: Physics