Electron capture cross sections and nuclear partition functions for fp-shell nuclei

Abstract

We present calculation of electron capture cross sections (ECC), in the limit of zero momentum transfer, using the pn QRPA model in stellar matter. Towards this aim we make use of our recently introduced recipe for estimation of nuclear partition functions. For low momentum transfer q tends to zero, the nuclear matrix elements of the Pστ plus operator provide the leading contribution to the total cross section which we estimate using the pn QRPA model in a multi shell single particle space with a schematic interaction. Key f p shell nuclei (odd A, even even and odd odd) bearing astrophysical importance were selected for the calculation of ECC in stellar environment. These f p shell nuclei play crucial role in pre supernova evolution of massive stars and core collapse. We further present microscopic calculation of ground and excited states Gamow Teller strength distributions and stellar electron capture rates on these suite of nuclei. We used two different sets of empirically determined pairing gaps to calculate the ECC and electron capture rates. Results are compared with experimental data and previous computations. Our calculated ECC are systematically smaller at low electron incident energies as compared to the shell model results.

19 Page, 5 Tables, 9 Figures

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• Nuclear Partition Functions at Temperatures Exceeding 10^10 K
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• Impact of the Brink Axel Hypothesis on Unique First Forbidden \b{eta} transitions for r process nuclei
• Nuclear structure properties and weak interaction rates of even-even Fe isotopes
• Energy rates due to Fe isotopes during presupernova evolution of massive stars
• Investigation of weak-rates for odd-A nuclei for presupernova simulations