Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...265..429c&link_type=abstract
Astrophysical Journal, Part 1, vol. 265, Feb. 1, 1983, p. 429-442. Research supported by the University of Oklahoma
Astronomy and Astrophysics
Astrophysics
29
B Stars, Helium, Nuclear Fusion, Stellar Models, Supernovae, Carbon Isotopes, Decay Rates, Neon Isotopes, Neutron Sources, Oxygen Isotopes, Shock Waves
Scientific paper
The consequences of shock heating of the helium zone in a star undergoing a supernova explosion is examined for a wide variety of temperatures, densities, and shock velocities. It is found that for peak densities near 10,000 g/cu cm and a rather narrow range of temperatures around 4 x 10 th the 8th K, the solar system r-process abundance curve is reproduced. These conditions correspond to shock wave velocities of approximately 4000 km/s in the helium zone of an evolved star. The neutron source for this helium-driven r-process is C-13. It is suggested that the C-13 abundance in the helium zone could be produced in sufficient quantities by some type of mixing or dredging process between the hydrogen-rich envelope and the helium zone. The calculated fit to the solar system r-process curve is improved when the beta decay rates of the heavy nuclei are increased by a factor of 5-10 over the rates using the gross theory.
Cameron G. W. A.
Cowan John J.
Truran Jame. W.
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