EDP Sciences
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Volume 441, Number 3, October III 2005
Page(s) 1129 - 1133
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20053084

A&A 441, 1129-1133 (2005)
DOI: 10.1051/0004-6361:20053084

Influence of two updated nuclear reaction rates on the evolution of low and intermediate mass stars

A. Weiss1, A. Serenelli2, 1, A. Kitsikis1, H. Schlattl1 and J. Christensen-Dalsgaard3

1  Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
    e-mail: weiss@mpa-garching.mpg.de
2  Institute for Advanced Study, Einstein Drive, Princeton NJ 08540, USA
3  Institut for Fysik og Astronomi, Aarhus Universitet, Bygn. 520, Ny Munkegade, 8000 Aarhus C, Denmark

(Received 18 March 2005 / Accepted 19 July 2005 )

Two key reactions of hydrostatic nuclear burning in stars have recently been revised by new experimental data - the $^{14}{\rm N}(p,\gamma)^{15}{\rm0}$ and $3\,\alpha$ reaction rates. We investigate how much the new rates influence the evolution of low-mass, metal-poor and metal-free stars and of an intermediate-mass star of solar-type composition. We concentrate on phases of helium ignition or thermally unstable helium burning. Our global result is that the new $3\,\alpha$ rate has no significant influence on such stars, but that there is a noticeable though small effect of the new $^{14}{\rm N}(p,\gamma)^{15}{\rm0}$ rate, in particular on the core helium flash and the blue loop during core helium burning in the intermediate-mass star.

Key words: stars: interiors -- stars: evolution -- nuclear reactions, nucleosynthesis, abundances

© ESO 2005