Nuclear data needs for the study of nucleosynthesis in massive stars

Woosley, S. E. and Heger, A. and Rauscher, T. and Hoffman, R. D.. (2003) Nuclear data needs for the study of nucleosynthesis in massive stars. Nuclear physics. A, Nuclear and hadronic physics, Vol. 718 , S. 3C-12C.

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Official URL: http://edoc.unibas.ch/dok/A5839276

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The critical nuclear physics needed to calculate the evolution of and nucleosynthesis in massive stars is reviewed with emphasis on the uncertainties. Some reaction rates - the most important and uncertain still being C-12 (alpha, gamma)O-16 - are important for energy generation and stellar structure. Others, like Ne-22(alpha,n)Mg-25 and individual cross sections for neutron capture determine the overall yield and distribution of the s-process for elements lighter than A = 90. Still others affect the synthesis of individual nuclei, e.g., by the nu-process, the rp-process, and the gamma-process. Weak interaction rates are important in determining the structure of both the pre-collapse and the post-collapse supernova core. Finally, both the site for, and the nuclear physics of the r-process remains very uncertain, quite possibly because of the neglect of magnetic fields.
Faculties and Departments:05 Faculty of Science > Departement Physik > Former Organization Units Physics > Theoretische Physik Astrophysik (Thielemann)
UniBasel Contributors:Rauscher, Thomas
Item Type:Article, refereed
Article Subtype:Research Article
Publisher:North Holland
Note:Publication type according to Uni Basel Research Database: Journal article
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Last Modified:14 Sep 2012 07:18
Deposited On:14 Sep 2012 06:44

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