Volume 522, November 2010
|Number of page(s)||10|
|Section||Stellar structure and evolution|
|Published online||28 October 2010|
Electron fraction constraints based on nuclear statistical equilibrium with beta equilibrium
Institut für Kernphysik, Technische Universität Darmstadt,
2 GSI Helmholtzzentrum für Schwerionenforschung GmbH, Planckstr. 1, 64291 Darmstadt, Germany
3 Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
Accepted: 15 July 2010
The electron-to-nucleon ratio or electron fraction is a key parameter in many astrophysical studies. Its value is determined by weak-interaction rates that are based on theoretical calculations subject to several nuclear physics uncertainties. Consequently, it is important to have a model independent way of constraining the electron fraction value in different astrophysical environments. Here we show that nuclear statistical equilibrium combined with beta equilibrium can provide such a constraint. We test the validity of this approximation in presupernova models and give lower limits for the electron fraction in type Ia supernova and accretion-induced collapse.
Key words: equation of state / stars: abundances / stars: evolution / supernovae: general
© ESO, 2010
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