Crust Composition and the Shallow Heat Source in KS 1731–260

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Abstract
The presence of a strong shallow heat source of unknown origin in accreting neutron star crusts has been inferred by analyzing x-ray observations of their cooling in quiescence. We model the cooling of KS 1731-260 using realistic crust compositions and nuclear heating and cooling sources from detailed nuclear reaction network calculations. We find that the required strength of the shallow heat source in KS 1731-260 is reduced by more than a factor of 3 compared to previous analysis, a 5σ difference that alleviates the need for exotic solutions. Our analysis also suggests the existence of an impure nuclear pasta layer in the inner crust of KS 1731-260, though future observations will provide more stringent constraints. In addition, we obtain constraints on the dominant surface burning modes of KS 1731-260 over its history.
Funding Information
  • National Science Foundation (PHY-1430152, OISE-1927130, PHY-1913554, PHY-2209429)
  • U.S. Department of Energy
  • Office of Science
  • Nuclear Physics (DE-SC0013037)
  • National Aeronautics and Space Administration (80NSSC20K0503)
  • Lawrence Livermore National Laboratory (DE-AC52-07NA27344)

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