Convective Instability in Hot Bubble in a Delayed Supernova Explosion

Details Convective Instability in Hot Bubble in a Delayed Supernova Explosion Convective Instability in Hot Bubble in a Delayed Supernova Explosion

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pthph..89.1175y&link_type=abstract

Progress of Theoretical Physics, Vol. 89, No. 6, pp. 1175-1182.

Physics

14

Scientific paper

Convective Instability behind a stalled shock wave is studied by performing a series of two-dimensional numerical simulations. This instability is induced by negative entropy gradient which is commonly formed in so-called `hot bubble' behind a stalled shock where matters are nearly hydrostatic and in radiative equilibrium. It is shown that an initial velocity perturbation of 1% of the sound velocity grows to be a nonlinear fluctuation in ~100 ms. It is possible that this bubble instability becomes a seed of the Rayleigh-Taylor instability in the stellar envelope if the shock revives. It is also shown, however, that in actual fact the convective instability does not power the shock enough to change the way of its propagation. Rotation (the centrifugal force is at most 5% of the gravitational force) does not affect the way of growth of the instability seriously either no matter what the initial rotation law is.

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