Postexplosion hydrodynamics of supernovae in red supergiants

Details Postexplosion hydrodynamics of supernovae in red supergiants Postexplosion hydrodynamics of supernovae in red supergiants

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...425..814h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 425, no. 2, p. 814-828

Astronomy and Astrophysics

Astrophysics

83

Flow Stability, Mixing, Shock Wave Propagation, Supergiant Stars, Supernovae, Two Fluid Models, Density Distribution, Perturbation Theory, Pressure Effects, Stellar Mass Ejection, Taylor Instability

Scientific paper

Shock propagation, mixing, and clumping are studied in the explosion of red supergiants as Type II supernovae using a two-dimensional smooth particle hydrodynamic (SPH) code. We show that extensive Rayleigh-Talor instabilities develop in the ejecta in the wake of the reverse shock wave. In all cases, the shell structure of the progenitor is obliterated to leave a clumpy, well-mixed supernova remnant. However, the occurrence of mass loss during the lifetime of the progenitor can significantly reduce the amount of mixing. These results are independent of the Type II supernova explosion mechanism.

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