| Issue |
A&A
Volume 522, November 2010
|
|
|---|---|---|
| Article Number | A25 | |
| Number of page(s) | 10 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/201014276 | |
| Published online | 28 October 2010 | |
Electron fraction constraints based on nuclear statistical equilibrium with beta equilibrium
1
Institut für Kernphysik, Technische Universität Darmstadt,
Schlossgartenstr. 9,
64289
Darmstadt
Germany
e-mail: a.arcones@gsi.de
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
Received:
17
February
2010
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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