Hydrodynamic instabilities in supernova remnants - Self-similar driven waves

Details Hydrodynamic instabilities in supernova remnants - Self-similar driven waves Hydrodynamic instabilities in supernova remnants - Self-similar driven waves

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...392..118c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 392, no. 1, June 10, 1992, p. 118-130.

Astronomy and Astrophysics

Astrophysics

134

Interstellar Matter, Magnetohydrodynamic Stability, Shock Waves, Supernova Remnants, Perturbation Theory, Shock Fronts, Spherical Harmonics, Stellar Winds, Supernovae

Scientific paper

An initial study aimed at elucidating the multidimensional aspects of the hydrodynamic instabilities in supernova remnants is presented. Self-similar solutions are found to exist for the interaction of a steep power-law density profile expanding into a relatively flat stationary power-law density profile. Consideration of the pressure and entropy profiles in the shocked 1D flows shows that the flows are subject to convective instability, by a local criterion. The growth rate for the instability becomes very large near the contact discontinuity between the two shocked regions. A linear analysis of the complete self-similar solutions shows that the solutions are unstable above a critical wavenumber and that the growth rate is greatest at the position of the contact discontinuity. The X-ray image of the remnant of SN 1572 (Tycho) shows emission from clumps of supernova ejecta, which is good evidence for instabilities in this remnant.

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