Presupernova collapse models with improved weak-interaction rates

2000/07/27 by A. Heger, K. Langanke, G. Martinez-Pinedo +1 · 3 citations
Physics and Astronomy · #astro-ph #nucl-th

paper · pdf · doi:10.1103/physrevlett.86.1678

published as Phys.Rev.Lett. 86 (2001) 1678-1681 · 4 pages, 2 figures

arxiv created 2000/07/27 · arxiv updated 2009/12/01

Abstract

Improved values for stellar weak interaction rates have been recently calculated based upon a large shell model diagonalization. Using these new rates (for both beta decay and electron capture), we have examined the presupernova evolution of massive stars in the range 15-40 Msun. Comparing our new models with a standard set of presupernova models by Woosley and Weaver, we find significantly larger values for the electron-to-baryon ratio Ye at the onset of collapse and iron core masses reduced by approximately 0.1 Msun. The inclusion of beta-decay accounts for roughly half of the revisions, while the other half is a consequence of the improved nuclear physics. These changes will have important consequences for nucleosynthesis and the supernova explosion mechanism.

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