TYPE Ib SUPERNOVA 2008D ASSOCIATED WITH THE LUMINOUS X-RAY TRANSIENT 080109: AN ENERGETIC EXPLOSION OF A MASSIVE HELIUM STAR-猫眼课题宝

DOI：

10.1088/0004-637x/692/2/1131

发表时间：

2008-07

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

Masaomi Tanaka;Masaomi Tanaka;N. Tominaga;K. Nomoto;K. Nomoto;S. Valenti;D. Sahu;T. Minezaki;Y. Yoshii;M. Yoshida;G. Anupama;S. Benetti;G. Chincarini;M. Valle;P. Mazzali;P. Mazzali;E. Pian

我们提出了超新星SN 2008 D与发光X射线瞬态080109的理论模型。根据流体动力学/核合成计算得到的先驱模型和爆炸模型，模拟了SN的热光变曲线和光谱。我们发现SN 2008 D是一个比正常的核心坍缩超新星更有能量的爆炸，其喷出物质量为Mej = 5.3 ± 1.0 M，动能为EK = 6.0 ± 2.5 × 1051 erg。SN的祖先星星在爆炸前有一个6-8 M的He核，基本上没有H包层（<5 × 10−4 M）。母星的主序星质量估计为MMS = 20-25 M，由于对流、质量损失、旋转和双星效应，还有额外的系统不确定性。这些性质介于正常超新星和与伽马射线爆发相关的超新星之间。中心残骸的质量估计为1.6-1.8 M，接近中子星星和黑洞形成的边界。

We present a theoretical model for supernova SN 2008D associated with the luminous X-ray transient 080109. The bolometric light curve and optical spectra of the SN are modeled based on the progenitor models and the explosion models obtained from hydrodynamic/nucleosynthetic calculations. We find that SN 2008D is a more energetic explosion than normal core-collapse supernovae, with an ejecta mass of Mej = 5.3 ± 1.0 M☉ and a kinetic energy of EK = 6.0 ± 2.5 × 1051 erg. The progenitor star of the SN has a 6–8 M☉ He core with essentially no H envelope (<5 × 10−4 M☉) prior to the explosion. The main-sequence mass of the progenitor is estimated to be MMS = 20–25 M☉, with additional systematic uncertainties due to convection, mass loss, rotation, and binary effects. These properties are intermediate between those of normal SNe and hypernovae associated with gamma-ray bursts. The mass of the central remnant is estimated as 1.6–1.8 M☉, which is near the boundary between neutron star and black hole formation.

TYPE Ib SUPERNOVA 2008D ASSOCIATED WITH THE LUMINOUS X-RAY TRANSIENT 080109: AN ENERGETIC EXPLOSION OF A MASSIVE HELIUM STAR

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