Microscopic calculations of weak interaction rates of nuclei in stellar environment for A = 18 to 100

J.-U. Nabi; H.V. Klapdor-Kleingrothaus

doi:doi:10.1007/s100500050292

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2018 Impact factor 2.481

Hadrons and Nuclei

Eur. Phys. J. A 5, 337-339

Microscopic calculations of weak interaction rates of nuclei in stellar environment for A = 18 to 100

J.-U. Nabi - H.V. Klapdor-Kleingrothaus

Max-Planck-Institut für Kernphysik, D-69029 Heidelberg, Germany

Received: 16 April 1999 Communicated by B. Povh

Abstract
We report here the microscopic calculation of weak interaction rates in stellar matter for 709 nuclei with A = 18 to 100 using a generalized form of proton-neutron quasiparticle RPA model with separable Gamow-Teller forces. This is the first ever extensive microscopic calculation of weak rates calculated over a wide temperature-density grid which includes 10⁷ $\leq$ T(K) $\leq$ 30 $\times$ 10⁹ and 10 $\leq$ $\rho Y_{e}$ (gcm^-3) $\leq$ 10¹¹, and over a larger mass range. Particle emission processes from excited states, previously ignored, are taken into account, and are found to significantly affect some $\beta$ decay rates. The calculated capture and decay rates take into consideration the latest experimental energy levels and ft value compilations. Our calculation of electron capture and $\beta$ -decay rates, in the fp-shell, show considerable differences with a recently reported shell model diagonalization approach calculation.

PACS
23.40.-s $\beta$ decay; double $\beta$ decay; electron and muon capture - 23.40.Bw Weak-interaction and lepton (including neutrino) aspects - 21.60.Jz Hartree-Fock and random-phase approximations