Thermonuclear kinetics in astrophysics
نویسندگان
چکیده
منابع مشابه
Se p 20 05 Thermonuclear Kinetics in Astrophysics
Over the billions of years since the Big Bang, the lives, deaths and afterlives of stars have enriched the Universe in the heavy elements that make up so much of ourselves and our world. This review summarizes the methods used to evolve these nuclear abundances within astrophysical simulations. These methods fall into 2 categories; evolution via rate equations and via equilibria. Because the ra...
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Recent improvements and remaining problems in the prediction of thermonuclear rates are reviewed. The main emphasis is on statistical model calculations, but the challenge to include direct reactions close to the driplines is also briefly addressed. Further theoretical as well as experimental investigations are motivated.
متن کاملar X iv : a st ro - p h / 05 09 69 8 v 1 22 S ep 2 00 5 Thermonuclear Kinetics in Astrophysics
Over the billions of years since the Big Bang, the lives, deaths and afterlives of stars have enriched the Universe in the heavy elements that make up so much of ourselves and our world. This review summarizes the methods used to evolve these nuclear abundances within astrophysical simulations. These methods fall into 2 categories; evolution via rate equations and via equilibria. Because the ra...
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The prediction of cross sections for nuclei far off stability is crucial in the field of nuclear astrophysics. In recent calculations the nuclear level density – as an important ingredient to the statistical model (Hauser-Feshbach) – has shown the highest uncertainties. We present a global parametrization of nuclear level densities based on the back-shifted Fermi-Gas formalism. Employment of an...
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It has recently been argued that there are no dynamic screening corrections to Salpeter’s enhancement factor in thermonuclear reactions, in the weak-screening limit. The arguments used were: 1) The Gibbs probability distribution is factorable into two parts, one of which, exp(−β∑ eiej/rij) (β = 1/kBT ), is independent of velocity space; and 2) The enhancement factor is w = 1 + βeZ1Z2〈φ〉 with 〈φ...
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ژورنال
عنوان ژورنال: Nuclear Physics A
سال: 2006
ISSN: 0375-9474
DOI: 10.1016/j.nuclphysa.2004.10.009