AAS 199th meeting, Washington, DC, January 2002
Session 67. Supernovae
Oral, Tuesday, January 8, 2002, 10:00-11:30am, International Ballroom East

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[67.04] Spherically Symmetric Core Collapse Supernova Simulations With Boltzmann Neutrino Transport

O. E. B. Messer (University of Tennessee/ORNL)

I will describe the results of several spherically symmetric core collapse supernova simulations performed with AGILE-BOLTZTRAN, a state-of-the-art radiation hydrodynamics code incorporating Boltzmann neutrino transport.

Collapse simulations comparing two 15 M\sun progenitor models with significant differences in initial Ye (Woosley & Weaver 1995, Heger et al. 2000) exhibit no differences in Ye at bounce, and, consequently, no difference in homologous core mass and shock formation radius. Fully dynamic simulations of core collapse, rebound, and shock propagation for 15 M\sun and 20 M\sun progenitor models of Nomoto & Hashimoto (1988) fail to produce explosions. In both cases, the shock stalls at ~ 200 km, then recedes for several hundred milliseconds.

The marked similarities observed in all these simulations highlight the need for both improved progenitor models and the incorporation of improved microphysics in modern supernova codes. Spherically symmetric simulations are, for the immediate future, the only computationally feasible way to investigate the nature of the explosion mechanism while including the requisite level of detailed neutrino transport. They also provide one of the few opportunities to delineate the effects of various feedback mechanisms present in the problem.

This research was supported by funds from the Joint Institute for Heavy Ion Research and a DOE PECASE award, and made use of the resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC03-76SF00098.

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The author(s) of this abstract have provided an email address for comments about the abstract: bmesser@utk.edu

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