Nuclear reaction rates and opacity in massive star evolution calculations

0481889 - ASÚ 2018 RIV US eng C - Konferenční příspěvek (zahraniční konf.)
Bahena, David - Klapp, J. C. - Dehnen, H.
Nuclear reaction rates and opacity in massive star evolution calculations.
Proceedings of the 33rd Symposium on Nuclear Physics. Bristol: Institute of Physics Publishing, 2010, 012004/1-012004/8. Journal of Physics Conference Series, 239. ISSN 1742-6588.
[Symposium on Nuclear Physics /33./. Morelos (MX), 05.01.2010-08.01.2010]
Výzkumný záměr: CEZ:AV0Z10030501
Klíčová slova: thermonuclear reaction-rates * m-circle-dot * rosseland mean opacity
Obor OECD: Astronomy (including astrophysics,space science)

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 200 M-circle dot galactic and pregalactic stars with metallicity Z = 10(-6) and 10(9), 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.
Trvalý link: http://hdl.handle.net/11104/0277347