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S. A. Colgate, R. H. White. The hydrodynamic behavior of su- pernovae explosions. The Astrophysical Journal, 1966, 143: 626- 681.


  • 标题: 11~40MΘ前新星模型下的II型超新星爆发能研究Research on Explosion Energy of Type II-Supernova in 11~40MΘ Progenitor Stars Model

    作者: 夏雄平

    关键字: 前新星, 爆发能, II型超新星Progenitor Stars; Explosion Energy; Type II-Supernova

    期刊名称: 《Astronomy and Astrophysics》, Vol.1 No.2, 2013-04-30

    摘要: 本文通过采用四种爆发能的定义,修正了LLPR模型中与爆发能相关的状态方程和II型超新星爆发的模拟程序“WLYW-89”,模拟了最近修正的主序质量在(:太阳质量)的前新星模型数据下的II型超新星的爆发。根据不同壳层下离散的爆发能和随时间变化的爆发能特征,同时对比实验观测的数据。研究结果显示,在四种不同的爆发能定义中,定义是比较符合当前前新星的模型数据,特别是对于中小质量的前新星,模拟结果与实验结果符合比较好。它主要体现在其定义从能量观点进行定义,其激波速度符合实验观测数据,并能缩小理论与实验观测结果的差距。In the paper, we apply four various definitions of explosion energy, based on modified the state equation in LLPR model and the II supernova explosion code “WLYW-89”, to research explosion energy of type II-supernova in new progenitor stars model of the main-sequence mass (: the sun mass). Apply the results of the discrete explosion energy in various mass cell and explosive energy with time, and compare with theoretical and observation results, we find that, in four various definitions of explosion energy, the second definition of explosion energy is the most suitable to supernova explosion in new progenitor stars model, especially, for , theoretical results are good agreement with experimental observation data. It is because that, on one the hand, is defined by the view of energy, on the other hand, its shock velocity in agreement with the experimental observation and it can reduce the gap of theoretical and observation results.