Early expansion and luminosity evolution of supernovae
Early expansion and luminosity evolution of supernovae
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DOI：
10.1086/171612
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发表时间：
1992-08
期刊：
影响因子：
--
通讯作者：
R. Chevalier
中科院分区：
文献类型：
--
作者：
R. Chevalier
超新星的初始平面膨胀可以用一个自相似解来描述，如果它的祖恒星足够致密，在这个阶段辐射转移效应不起重要作用。后来气体的自由膨胀导致密度和压力分布的径向幂律，尽管球面几何的影响使这个结果有些不准确。如果最初的膨胀确实建立了密度和压力的幂定律，那么辐射扩散的影响可以用一个自相似的扩散波来描述，扩散波返回到气体中
The initial planar expansion of a supernova can be described by a self-similar solution if the progenitor star is sufficiently compact that radiative transfer effects do not play an important role during this phase. The later free expansion of the gas leads to radial power laws for the density and pressure profiles, although the effects of spherical geometry give some inaccuracy in this result. If the initial expansion does set up power laws for the density and pressure, effects of radiative diffusion can be described by a self-similar diffusion wave that moves back into the gas