General relativistic hydrodynamics and the adiabatic collapse of stellar cores
General relativistic hydrodynamics and the adiabatic collapse of stellar cores
复制标题
广义相对论流体动力学和恒星核心的绝热塌缩
DOI：
10.1086/157314
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发表时间：
1979
期刊：
影响因子：
--
通讯作者：
K. Riper
中科院分区：
文献类型：
--
作者：
K. Riper
利用广义相对论研究了大质量星星球对称铁核的坍缩和超新星爆发，通过核-反弹-反射-激波机制。在最近的一些崩塌计算中，尽管Gr的“修正”看起来很小，但忽略了Gr是不合理的。低密度下的反弹（rho/sub c/约=10/sup 13/ g cm/sup-3/），在GR中接近临界，可能不会发生。使用兰姆、拉蒂默、佩西克和拉文霍尔的新状态方程，塌缩模拟在超过核密度之前不会显示反弹。给出了在中子星星密度处反弹的坍缩模型的结果。大爆炸能量-高达6 × 10/sup 51/ ergs-被发现，如果反弹是近临界的状态方程的GR“有效软化”，然后导致大的反弹幅度所需的能量爆炸的流体动力学机制。考虑了中子星和黑洞形成之间的质量划分。给出了GR流体动力学的差分方程。
The collapse and supernova explosion, via the core-bounce--reflection-shock mechanism, of a spherically symmetric, iron core of a massive star is studied using the full general theory of relativity (GR). The neglect of GR in some recent collapse calculations is not justified, even though the Gr ''corrections' appear small. Bounces at low density (rho/sub c/approx. =10/sup 13/ g cm/sup -3/), which are found in these Newtonian models, are close to critical in GR, and may not occur. With the new equation of state of Lamb, Lattimer, Pethick, and Ravenhall, collapse simulations will not show a bounce until nuclear density is exceeded. The results of collapse models which bounce at neutron star densities are presented. Large explosion energies--up to 6 x 10/sup 51/ ergs--are found if the bounce is near critical; the GR ''effective softening'' of the equation of state then leads to the large rebound amplitude necessary for energetic explosions by the hydrodynamic mechanism. The mass division between neutron-star and black-hole formation is considered. The difference equations used for the GR hydrodynamics are presented.