Motivated by observations of supernova SN 1987A, various authors have
simulated Rayleigh-Taylor (RT) instabilities in the envelopes of core collapse
supernovae (for a review, see Mueller 1998). The non-radial motion found in
these simulations qualitatively agreed with observations in SN 1987A, but
failed to explain the extent of mixing of newly synthesized 56Ni
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.Comment: 4 pages, 1 figure, LaTeX, requires espcrc1.sty. To appear in Nucl.
Phys. A., the proceedings of the conference "Nuclei in the Cosmos 2000", held
in Aarhus, Denmark, June 27-July 1, 200