Convective supernovae

Details Convective supernovae Convective supernovae

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...139..368b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 139, no. 2, Oct. 1984, p. 368-374.

Astronomy and Astrophysics

Astrophysics

40

Convection, Density Distribution, Supernovae, Differential Equations, Eigenvalues, Explosions, Taylor Instability

Scientific paper

The onset of instabilities during the first phases of supernova explosions, when the material is still optically thick and radiation dominated, is studied theoretically. Convection appears to be much more effective than the Rayleigh-Taylor instability, which has been considered in the past. A class of self-similar analytical solutions is used for the explosion in a medium with a power law density distribution to evaluate the effectiveness of convection. It is found, for a slope of the original density profile close to -3, that convection not only saturates, but also noticeably affects the dynamics of the explosion. A slope close to -3 is in fact in general agreement with models of high mass, radiation dominated stars, which are commonly accepted as Type II supernova progenitors.

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