1999/07/29 by Jameel‐Un Nabi, J. -U Nabi, Nabi, J. -U +3
Physics and Astronomy · #Astro and Planetary Science #FOS: Physical sciences #Nuclear Theory (nucl-th) #Nuclear physics research studies #Quantum, superfluid, helium dynamics #nucl-th
paper · pdf · doi:10.48550/arxiv.nucl-th/9907112
119 pages, 35 figures, rates are presented on an abbreviated scale to save space
arxiv created 1999/07/29 · openalex publication_date 1999/07/29 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Nuclear weak interaction rates for fp-shell nuclei in stellar matter and the associated energy losses are calculated using a modified form of proton-neutron quasiparticle RPA model with separable Gamow-Teller forces. The stellar weak rates are calculated over a wide range of densities (10 < ρYe (gcm-3) < 1011) and temperatures (107 < T(K) < 30 x 109). This is the first ever extensive compilation of weak interaction rates in stellar matter calculated over a wide temperature-density grid and over a larger mass range. The calculated capture and decay rates take into consideration the latest experimental energy levels and ft value compilations. We have calculated stellar weak interaction rates for a total of 619 nuclei in the mass range A = 40 to 100. These also include many important neutron-rich nuclei which play an important role in the evolution process of stellar collapse. This is our second paper in a series where we will be presenting our results on an abbreviated scale of temperature and density for the mass range A = 18 to 100. This paper contains the stellar weak rates in the mass range 40 to 60.