On the Rayleigh-Taylor instability in stellar explosions

Details On the Rayleigh-Taylor instability in stellar explosions On the Rayleigh-Taylor instability in stellar explosions

Feb 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...219..994c&link_type=abstract

Astrophysical Journal, Part 1, vol. 219, Feb. 1, 1978, p. 994-1007.

Astronomy and Astrophysics

Astrophysics

49

Explosions, Stellar Mass Ejection, Supernovae, Taylor Instability, Adiabatic Conditions, Elastic Waves, Hydrodynamics, Novae, Shock Wave Propagation, Stellar Envelopes

Scientific paper

After a shock wave has accelerated the outer layers of a star during a stellar explosion, a rarefaction wave moves back into the stellar material, resulting in the conversion of internal energy into kinetic energy. This additional acceleration can be Rayleigh-Taylor unstable. Two-dimensional hydrodynamic calculations are presented for the case of Type II supernovae, showing that the instability results in the ejection of a clumpy shell. It is unlikely that radiation transport can damp the instability for normal Type II supernovae. We further conjecture that the structure of nova shells is a consequence of this instability; in this case, rings are formed by the smearing action of high rotational velocities.

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