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I.K. Heyward, J.M. Blondin (NC State University), A. Mezzacappa (Oak Ridge National Lab), TeraScale Supernova Initiative Collaboration
Building on previous hydrodynamic simulations of the post-bounce phase of core collapse supernovae, we introduce self gravity into the model and allow the stellar core to evolve with the simulation. In the original models of the SASI, the stellar core was modeled with a fixed reflecting boundary at the surface of the proto-neutron star and the gravitational force was treated as a fixed point source. Here we replace the fixed core with a polytrope of index n=2/3, and use a Poisson solver to compute the self gravity of both the polytrope and the accreting gas. This modification allows us to quantitatively measure the motion of the proto-neutron star induced by the SASI as well as any possible feedback of the moving core on the growth of the SASI.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.