Improved Nuclear Physics Near $A=61$ Refines Urca Neutrino Luminosities in Accreted Neutron Star Crusts

Abstract

We performed a Penning trap mass measurement of ${}^{61}\mathrm{Zn}$ at the National Superconducting Cyclotron Laboratory and NuShellX calculations of the ${}^{61}\mathrm{Zn}$ and ${}^{62}\mathrm{Ga}$ structure using the GXPF1A Hamiltonian to obtain improved estimates of the ${}^{61}\mathrm{Zn}(p,\gamma {)}^{62}\mathrm{Ga}$ and ${}^{60}\mathrm{Cu}(p,\gamma {)}^{61}\mathrm{Zn}$ reaction rates. Surveying astrophysical conditions for type-I X-ray bursts with the code MESA, implementing our improved reaction rates, and taking into account updated nuclear masses for ${}^{61}\mathrm{V}$ and ${}^{61}\mathrm{Cr}$ from the recent literature, we refine the neutrino luminosity from the important mass number $A=61$ urca cooling source in accreted neutron star crusts. This improves our understanding of the thermal barrier between deep heating in the crust and the shallow depths where extra heat is needed to explain X-ray superbursts, as well as the expected signature of crust urca neutrino emission in light curves of cooling transients.

Submitted

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Cited by in corpus (3)

• Impacts of the direct URCA and Superfluidity inside a Neutron Star on Type-I X-Ray Bursts and X-Ray Superbursts
• Constraining Accreted Neutron Star Crust Shallow Heating with the Inferred Depth of Carbon Ignition in X-ray Superbursts
• Nuclear astrophysics