Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992ianp.symp..281t&link_type=abstract
Symposium on the Interface of Astrophysics with Nuclear and Particle Physics, p. 281 - 315
Astronomy and Astrophysics
Astrophysics
Scientific paper
In the following a brief introduction is given to the physics in astrophysical plasmas which governs composition changes. The author presents the basic equations for thermonuclear reaction rates and nuclear reaction networks. The required nuclear-physics input for reaction rates is discussed. After a brief review of hydrostatic burning stages in stellar evolution, he focuses on explosive burning. Discussed are the abundances resulting from the big bang and the nucleosynthesis in type I and II supernovae, which are linked either to white dwarfs in binary systems or to the gravitational collapse of massive stars at the end of their hydrostatic evolution. SN 1987A, the first type II supernova for which the progenitor star was known, is used as an example for nucleosynthesis calculations. Then, the author concentrates on the r-process, where a combination of the observed isotopic r-abundance pattern and nuclear-physics knowledge far from stability can be used to deduce the conditions required in an astrophysical production site. The connection of such conditions with present supernova models is discussed. Finally, he discusses explosive H-burning and the rp-process, occurring on white dwarfs and neutron stars in binary systems with low mass transfer rates.
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