Microscopic calculations of stellar weak interaction rates and energy losses for fp- and fpg-shell nuclei

Details Microscopic calculations of stellar weak interaction rates and energy losses for fp- and fpg-shell nuclei Microscopic calculations of stellar weak interaction rates and energy losses for fp- and fpg-shell nuclei

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004adndt..88..237n&link_type=abstract

Atomic Data and Nuclear Data Tables, Volume 88, Issue 2, p. 237-476.

Mathematics

Probability

29

Scientific paper

Nuclear weak interaction rates for fp- and fpg-shell nuclei in stellar matter and the associated energy losses are calculated using a modified form of proton neutron quasiparticle random phase approximation model with separable Gamow Teller forces. The stellar weak rates are calculated over a wide range of densities (10 ⩽ ρYe (g cm-3) ⩽ 1011) and temperatures (107 ⩽ T (K) ⩽ 30 × 109). We also calculate the probability of particle emission processes in stellar environment. We present an extensive compilation of weak interaction rates in stellar matter calculated over a wide temperature density grid and over a large mass range. The calculated capture and decay rates take into consideration the latest compilations of experimental energy levels and ft values. This paper is a follow up of our calculations introduced earlier [Eur. Phys. J. A 5 (1999) 337]. We have calculated stellar weak interaction rates for a total of 650 nuclei in the mass range A = 40 100. These also include many important neutron-rich nuclei which play an important role in the evolution process of stellar collapse.

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