Nuclear reaction rates and opacity in massive star evolution calculations

Details Nuclear reaction rates and opacity in massive star evolution calculations Nuclear reaction rates and opacity in massive star evolution calculations

Jul 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010jphcs.239a2004b&link_type=abstract

Journal of Physics: Conference Series, Volume 239, Issue 1, pp. 012004 (2010).

Physics

Scientific paper

Nuclear reaction rates and opacity are important parameters in stellar evolution. The input physics in a stellar evolution code determines the main theoretical characteristics of the stellar structure, evolution and nucleosynthesis of a star. For different input physics, in this work we calculate stellar evolution models of very massive first stars during the hydrogen and helium burning phases. We have considered 100 and 200M&sun; galactic and pregalactic stars with metallicity Z = 10-6 and 109, respectively. The results show important differences from old to new formulations for the opacity and nuclear reaction rates, in particular the evolutionary tracks are significantly affected, that indicates the importance of using up to date and reliable input physics. The triple alpha reaction activates sooner for pregalactic than for galactic stars.

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