The Type Ic Hypernova SN 2003dh/GRB 030329
The Type Ic Hypernova SN 2003dh/GRB 030329
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DOI：
10.1086/381259
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发表时间：
2003-09
期刊：
影响因子：
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通讯作者：
P. Mazzali;J. Deng;N. Tominaga;K. Maeda;K. Nomoto;T. Matheson;K. Kawabata;K. Stanek;P. Garnavich
中科院分区：
文献类型：
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作者：
P. Mazzali;J. Deng;N. Tominaga;K. Maeda;K. Nomoto;T. Matheson;K. Kawabata;K. Stanek;P. Garnavich
在GRB 030329的余辉中发现的SN 2003dh的光谱用辐射输运编码进行了建模。结果表明，SN 2003dh具有很高的爆炸动能（约4 × 1052尔格），使其成为迄今为止观测到的最强大的超新星之一，并支持了超新星与伽马射线暴之间的联系。然而，通过拟合光谱得出的光度曲线表明，SN 2003dh不如SN 1998bw明亮，仅喷射出56Ni的~0.35 M☉。SN 2003dh的光谱与SN 1998bw在最大值时的光谱相似，但后来它们看起来更像能量较低的超新星SN 1997ef。光谱和推断的光曲线可以采用类似于SN 1998bw在v - > - 25,000 km s-1时的密度分布来建模，但更接近SN 1997ef在较低速度下的密度分布。喷出物的质量约为8 M☉，比其他两个超超新星的质量略小。它的前身一定是一颗大质量恒星（M ~ 35-40 M☉），就像其他超超新星一样。需要结合不同的一维爆炸模型强烈表明SN 2003dh是一次不对称爆炸。
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☉ 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☉, somewhat less than in the other two hypernovae. The progenitor must have been a massive star (M ~ 35-40 M☉), as for other hypernovae. The need to combine different one-dimensional explosion models strongly indicates that SN 2003dh was an asymmetric explosion.