Rayleigh-Taylor instability and mixing in SN 1987A

Details Rayleigh-Taylor instability and mixing in SN 1987A Rayleigh-Taylor instability and mixing in SN 1987A

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...344l..65e&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 344, Sept. 15, 1989, p. L65-L68. Research supported by the Instit

Astronomy and Astrophysics

Astrophysics

48

Astronomical Models, Magnetohydrodynamics, Rayleigh Scattering, Shock Wave Propagation, Supernova 1987A, Taylor Instability, Pressure Distribution, Stellar Envelopes, Stellar Luminosity, Stellar Models

Scientific paper

The stability of the supernova ejecta is compared with the Rayleigh-Taylor instability for a realistic model of SN 1987A. A linear analysis indicates that the layers around the composition interface between the hydrogen-rich and helium zones, and become Rayleigh-Taylor unstable between the helium and metal zones. In these layers, the pressure increases outward because of deceleration due to the reverse shock which forms when the blast shock hits the massive hydrogen-rich envelope. On the contrary, the density steeply decreases outward because of the preexisting nuclear burning shell. Then, these layers undergo the Raleigh-Taylor instability because of the opposite signs of the pressure and density gradients. The estimated growth rate is larger than the expansion rate of the supernova. The Rayleigh-Taylor instability near the composition interface is likely to induce mixing, which has been strongly suggested from observations of SN 1987A.

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