TYPE IIn SUPERNOVA SN 2010jl: OPTICAL OBSERVATIONS FOR OVER 500 DAYS AFTER EXPLOSION

We present extensive optical observations of a Type IIn supernova (SN IIn) 2010j1 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. These...

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Bibliographic Details
Published inThe Astronomical journal Vol. 144; no. 5; pp. 131 - 13
Main Authors Zhang, Tianmeng, Wang, Xiaofeng, Wu, Chao, Chen, Juncheng, Chen, Jia, Liu, Qin, Huang, Fang, Liang, Jide, Zhao, Xulin, Lin, Lin, Wang, Min, Dennefeld, Michel, Zhang, Jujia, Zhai, Meng, Wu, Hong, Fan, Zhou, Zou, Hu, Zhou, Xu, Ma, Jun
Format Journal Article
LanguageEnglish
Published United States American Astronomical Society 01.11.2012
Subjects
Astronomical instruments
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
ASYMMETRY
BALMER LINES
COSMIC DUST
DIAGRAMS
EMISSION SPECTRA
EMISSION SPECTROSCOPY
Evolution
Explosions
Flattening
HYDROGEN
LUMINOSITY
MASS
RED SHIFT
Sciences of the Universe
Shells
STELLAR WINDS
SUPERGIANT STARS
SUPERNOVAE
Supernovas
VISIBLE RADIATION
Yield strength
supernovae: individual: SN 2010jl
supernovae: general
Astrophysics - Solar and Stellar Astrophysics
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Summary:We present extensive optical observations of a Type IIn supernova (SN IIn) 2010j1 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. 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. Considering a slow-moving stellar wind (e.g., ~28 km s-l) inferred for the preexisting, dense CSM shell and the extremely high mass-loss rate (1-2 M sub([odot]) yr super(-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 sub([odot]).
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ISSN:0004-6256
1538-3881
1538-3881
DOI:10.1088/0004-6256/144/5/131