Mazzali 2004 SN 2003dh 谱和光变

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Title:		The Type Ic Hypernova SN 2003dh/GRB 030329
Authors:		Mazzali, Paolo A.; Deng, Jinsong; Tominaga, Nozomu; Maeda, Keiichi; Nomoto, Ken'ichi; Matheson, Thomas; Kawabata, Koji S.; Stanek, Krzysztof Z.; Garnavich, Peter M.
Publication:		The Astrophysical Journal, Volume 599, Issue 2, pp. L95-L98. (ApJ Homepage)
Publication Date:		12/2003
Origin:		UCP
ApJ Keywords:		Gamma Rays: Bursts, Nuclear Reactions, Nucleosynthesis, Abundances, Stars: Supernovae: General, Stars: Supernovae: Individual: Alphanumeric: SN 2003dh
Abstract Copyright:		(c) 2003: The American Astronomical Society
DOI:		10.1086/381259
Bibliographic Code:		2003ApJ...599L..95M

Abstract

The spectra of SN 2003dh, identified in the afterglow of GRB 030329, are modeled using radiation transport codes. It is shown that SN 2003dh had a high explosion kinetic energy (~4×10⁵² ergs in spherical symmetry), making it one of the most powerful hypernovae observed so far and supporting the case for association between hypernovae and gamma-ray bursts. However, the light curve derived from fitting the spectra suggests that SN 2003dh was not as bright as SN 1998bw, ejecting only ~0.35 M_solar of ⁵⁶Ni. The spectra of SN 2003dh resemble those of SN 1998bw around maximum, but later they look more like those of the less energetic hypernova SN 1997ef. The spectra and the inferred light curve can be modeled adopting a density distribution similar to that used for SN 1998bw at v>25,000 km s^-1 but more like that of SN 1997ef at lower velocities. The mass of the ejecta is ~8 M_solar, somewhat less than in the other two hypernovae. The progenitor must have been a massive star (M~35-40 M_solar), as for other hypernovae. The need to combine different one-dimensional explosion models strongly indicates that SN 2003dh was an asymmetric explosion.

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