Effects of Beta-Decays of Excited-State Nuclei on the Astrophysical r-Process

Abstract

A rudimentary calculation is employed to evaluate the possible effects of beta- decays of excited-state nuclei on the astrophysical r-process. Single-particle levels calculated with the FRDM are adapted to the calculation of beta-decay rates of these excited-state nuclei. Quantum numbers are determined based on proximity to Nilson model levels. The resulting rates are used in an r-process network calculation in which a supernova hot-bubble model is coupled to an extensive network calculation including all nuclei between the valley of stability and the neutron drip line and with masses A<284. Beta-decay rates are included as functional forms of the environmental temperature. While the decay rate model used is simple and phenomenological, it is consistent across all 3700 nuclei involved in the r-process network calculation. This represents an approximate first estimate to gauge the possible effects of excited-state beta-decays on r-process freeze-out abundances.

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• New Nuclear Reaction Flow during r-Process Nucleosynthesis in Supernovae: Critical Role of Light Neutron-Rich Nuclei
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Cited by in corpus (6)

• The impact of individual nuclear properties on $r$-process nucleosynthesis
• Large scale evaluation of beta-decay rates of r-process nuclei with the inclusion of first-forbidden transitions
• Current Status of r-Process Nucleosynthesis
• r-Process Nucleosynthesis: Connecting Rare-Isotope Beam Facilities with the Cosmos
• The Gaia-ESO survey: placing constraints on the origin of r-process elements
• $\beta$-decay half-lives at finite temperatures for N=82 isotones