2002/11/12 by Jason Pruet, J Pruet, George M. Fuller · 4 citations
Physics and Astronomy · #Astrophysics #Atomic physics #Electron #Electron capture #Fermi Gamma-ray Space Telescope #Isobaric process #Neutrino #Neutrino Physics Research #Nuclear physics #Nuclear physics research studies #Partition (number theory) #Physics #Quantum Chromodynamics and Particle Interactions #Range (aeronautics) #astro-ph
paper · pdf · doi:10.1086/376753
Tables of rates for nuclei in the mass range A=66-110 are available from J. Pruet
arxiv created 2002/11/12 · openalex publication_date 2003/10/24 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We estimate lepton capture and emission rates, as well as neutrino energy loss rates, for nuclei in the mass range A = 65-80. These rates are calculated on a temperature/density grid appropriate for a wide range of astrophysical applications including simulations of late time stellar evolution and X-ray bursts. The basic inputs in our single-particle and empirically inspired model are (i) experimentally measured level information, weak transition matrix elements, and lifetimes, (ii) estimates of matrix elements for allowed experimentally unmeasured transitions based on the systematics of experimentally observed allowed transitions, and (iii) estimates of the centroids of the GT resonances motivated by shell model calculations in the fp shell as well as by ( n , p ) and ( p , n ) experiments. Fermi resonances (isobaric analog states) are also included, and it is shown that Fermi transitions dominate the rates for most interesting proton-rich nuclei for which an experimentally determined ground state lifetime is unavailable. For the purposes of comparing our results with more detailed shell model based calculations we also calculate weak rates for nuclei in the mass range A = 60-65 for which Langanke & Martinez-Pinedo have provided rates. The typical deviation in the electron capture and β-decay rates for these ≈30 nuclei is less than a factor of 2 or 3 for a wide range of temperature and density appropriate for presupernova stellar evolution. We also discuss some subtleties associated with the partition functions used in calculations of stellar weak rates and show that the proper treatment of the partition functions is essential for estimating high-temperature β-decay rates. In particular, we show that partition functions based on unconverged Lanczos calculations can result in errors in estimates of high-temperature β-decay rates.