Non-spherical core collapse supernovae and nucleosynthesis
نویسنده
چکیده
Motivated by observations of supernova SN1987A, various authors have simulated Rayleigh–Taylor (RT) instabilities in the envelopes of core collapse supernovae (for a review, see [1]). The non-radial motion found in these simulations qualitatively agreed with observations in SN1987A, but failed to explain the extent of mixing of newly synthesized Ni quantitatively. Here we present results of a 2D hydrodynamic simulation which re–addresses this failure and covers the entire evolution of the first 5 hours after core bounce.
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