Abstract
The propagation of spherical shock waves in the stellar interior is considered, extending the method developed in previous papers. A differential equation of the shock strength is derived, which can be applied to any stellar models. It is found that the spherical damping effect is pronounced near the center of stars, and this guarantees the stability of the stellar core in general. In the envelope, this effect becomes negligible, and it is justified near the stellar surface to treat the shock waves as plane.
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