Physics – Nuclear Physics
Scientific paper
Oct 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..dnp1wb001b&link_type=abstract
American Physical Society, Division of Nuclear Physics Fall Meeting, October 30 - November 1, 2003, Tucson, Arizona, MEETING ID:
Physics
Nuclear Physics
Scientific paper
An impediment to understanding the mechanism of the supernova explosions that attend the death of massive stars and the birth of pulsars is the numerical complexity of the solution of the equations of radiation transport and hydrodynamics. Codes to incorporate the dynamics, radiation transport, nuclear physics, equations of state, and nucleosynthesis in two and three spatial dimensions, in one energy (spectrum) dimension, and in one to two radiation angles all only now becoming feasible, but have yet to be constructed. Central to progress at this numerical frontier are efficient parallel algorithms to solve the coupled PDEs that describe the terminal evolution of these stars and visualization techniques that adequately capture the behavior of all of the relevant variables. I will discuss some of our past and present results in one and two spatial dimensions, including rotation, as well as plans for the future construction of multi-dimensional numerical tools to address this central problem in nuclear astrophysics.
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