arXiv 0905.11012009-05-07astro-ph.SR

初始太阳质量为23 - 33的超新星祖先星及其与SNR Cas A的关系

Supernova progenitor stars in the initial range of 23 to 33 solar masses and their relation with the SNR Cas A

B. Perez-Rendon, G. Garcia-Segura, N. Langer

备注：: 12 pages, 11 figures, accepted for publication in Astronomy & Astrophysics
DOI：: 10.1051/0004-6361/200809913

摘要：

仙后座A的多波长观测为我们提供了一个强有力的证据，证明在其母星周围存在星周物质。有人认为它的前身是一颗质量损失很大的大质量恒星。但是，尽管有大量的光学、红外、无线电和X射线观测数据，Cas A祖先的身份仍然难以捉摸。在这项工作中，我们计算恒星和拱星的数值模型来寻找Cas A的祖先。这些模型将与观测约束进行比较。我们计算了恒星演化模型，得到了随时间变化的风参数和表面丰度。我们已经选择了一组可能的祖星，初始质量为23，28，29，30和33 \Mo，质量损失。导出的质量损失率和风终极速度被用来模拟星周介质的演化。我们的恒星集给出了不同的SN祖先：RSG，发光蓝超巨星（LBSGs）和沃尔夫-拉叶（WR）星。23 \Mo恒星在$\rm ρ\sim r^{-2}$致密的自由流动风中爆炸为RSG，周围是薄的压缩RSG壳。28 $\Mo$恒星爆炸为LBSG，SN爆炸波与低密度的自由流动风相互作用，周围是不稳定的大质量“RSG + LBSG”壳。最后，30和33颗\Mo恒星爆炸为WR恒星，周围环绕着快速的WR风，终止于高度碎片化的“WR +RSG壳”。我们将我们的恒星模型的表面化学丰度与Cas A的观测丰度进行了比较。丰度分析显示，这颗恒星的初始质量约为30 \Mo，而流体动力学分析则认为这颗恒星的初始质量约为23。

英文摘要：

Multi wavelength observations of Cassiopeia A (Cas A) have provided us with a strong evidence for the presence of circumstellar material surrounding the progenitor star. It has been suggested that its progenitor was a massive star with a strong mass loss. But, despite the large amount of observational data from optical, IR, radio and x-ray observations, the identity of Cas A progenitor is still elusive. In this work, we compute stellar and circumstellar numerical models to look for the progenitor of Cas A. The models will be compared with the observational constraints. We have computed stellar evolution models to get time-dependent wind parameters and surface abundances. We have chosen a set of probable progenitor stars, with initial masses of 23, 28, 29, 30 and 33 \Mo, with mass loss. The derived mass loss rates and wind terminal velocities are used to simulate the evolution of the circumstellar medium. Our stellar set gives distinct SN progenitors: RSG, luminous blue super giants (LBSGs) and Wolf-Rayet (WR) stars. The 23 \Mo star explodes as a RSG in a $\rm ρ\sim r^{-2}$ dense, free streaming wind surrounded by a thin, compressed, RSG shell. The 28 $\Mo$ star explodes as a LBSG, and the SN blast wave interacts with a low density, free streaming wind surrounded by an unstable and massive ''RSG+LBSG'' shell. Finally, the 30 and 33 \Mo stars explode as WR stars surrounded by fast, WR winds that terminate in highly fragmented ''WR+RSG shell''. We have compared the surface chemical abundances of our stellar models with the observational abundances in Cas A. The abundance analysis shows that the progenitor was a star with an initial mass of the order of 30 \Mo, while the hydrodynamical analysis favors progenitors of initial masses around 23.

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