Convective instability of hollow Sedov-Taylor blast waves
Convective instability of hollow Sedov-Taylor blast waves
复制标题
空心谢多夫-泰勒冲击波的对流不稳定性
DOI：
10.1086/168977
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发表时间：
1990
期刊：
影响因子：
--
通讯作者：
J. Goodman
中科院分区：
文献类型：
--
作者：
J. Goodman
Sedov (1946) 和 Taylor (1950) 对于理想气体中强球形激波的自相似解，如果预激波密度下降为半径的高次幂，则其中心将被疏散。这些解决方案可以代表当冲击波穿过恒星包层时早期超新星爆炸波的理想形式。对于天体物理相关的绝热指数值，空心解对于全局对流模式是不稳定的；即瑞利-泰勒模式的可压缩推广。对于非常大的球谐函数 l，增长率按 l exp 1/2 缩放，并且特征函数集中在与流体内边缘的 1/l 成比例的距离内。还给出了局部对流不稳定性的条件，即使在不稳定的全局模态不存在时，该条件也可能存在。 36 参考文献
The self-similar solutions by Sedov (1946) and Taylor (1950) for a strong spherical shock in an ideal gas are evacuated at their centers if the preshock density falls as a high power of radius. These solutions could represent an idealized form of a supernova blast wave in the early phase when the shock moves through the stellar envelope. For astrophysically relevant values of the adiabatic index, the hollow solutions are unstable to global convective modes; that is, the compressible generalization of Rayleigh-Taylor modes. For very large spherical harmonic degrees l, the growth rate scales as l exp 1/2 and the eigenfunction is concentrated within a distance proportional to 1/l of the inner edge of the fluid. A condition is also given for local convective instability, which may exist even when unstable global modes to not. 36 refs.