Reaction models in nuclear astrophysics P.

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Reaction models in nuclear astrophysics P. Descouvemont Université Libre de Bruxelles, Brussels, Belgium 1 Introduction Reactions in astrophysics: general properties Reaction models Microcopic models The R-matrix method Conclusion 2 H, 4He

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01
Reaction models in nuclear astrophysics P. Descouvemont Université Libre de Bruxelles, Brussels, Belgium 1 Introduction
Reactions in astrophysics: general properties
Reaction models
Microcopic models
The R-matrix method
Conclusion<br>
02
2 H, 4He most abundant (~75%, ~25%)
« Gap » between A=4 and A=12: no stable element with A=5 and 8
Even-odd effects: nuclei with A even are more bound
Iron peak (very stable) Goal of nuclear astrophysics: understand the abundances of the elements 1. Introduction<br>
03
3 2. Reactions in astrophysics: general properties<br>