Weak shock propagation with accretion. III. a numerical study on shock propagation and stability

Stephen Ro, Eric R. Coughlin, Eliot Quataert

Research output: Contribution to journalArticlepeer-review

7 Scopus citations


Core-collapse supernovae span a wide range of energies, from much less than to much greater than the binding energy of the progenitor star. As a result, the shock wave generated from a supernova explosion can have a wide range of Mach numbers. In this paper, we investigate the propagation of shocks with arbitrary initial strengths in polytropic stellar envelopes using a suite of spherically symmetric hydrodynamic simulations. We interpret these results using the three known self-similar solutions for this problem: the Sedov-Taylor blast-wave describes an infinitely strong shock, and the self-similar solutions from Coughlin et al. (Papers I and II) describe a weak and infinitely weak shock (the latter being a rarefaction wave). We find that shocks, no matter their initial strengths, evolve toward either the infinitely strong or infinitely weak self-similar solutions at sufficiently late times. For a given density profile, a single function characterizes the long-term evolution of a shock's radius and strength. However, shocks with strengths near the self-similar solution for a weak shock (from Paper I) evolve extremely slowly with time. Therefore, the self-similar solutions for infinitely strong and infinitely weak shocks are not likely to be realized in low-energy stellar explosions, which will instead retain a memory of the shock strength initiated in the stellar interior.

Original languageEnglish (US)
Article number150
JournalAstrophysical Journal
Issue number2
StatePublished - Jun 20 2019
Externally publishedYes


  • Analytical - shock waves - supernovae
  • Black hole physics - hydrodynamics - methods
  • General

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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