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Crust Composition and the Shallow Heat Source in KS 1731-260.

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A new study on neutron star cooling suggests the shallow heat source in KS 1731-260 is weaker than previously thought. This finding reduces the need for exotic explanations and hints at nuclear pasta in the neutron star crust.

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Area of Science:

  • * Astrophysics
  • * Nuclear Physics
  • * Neutron Star Research

Background:

  • * Accreting neutron stars exhibit a strong shallow heat source in their crusts, inferred from X-ray cooling observations.
  • * The origin of this heat source in neutron star crusts remains largely unknown.
  • * Previous analyses required a significant heat source, prompting exotic explanations.

Purpose of the Study:

  • * To model the cooling of the neutron star KS 1731-260 using realistic crust compositions.
  • * To investigate the role of nuclear heating and cooling processes.
  • * To reassess the strength of the shallow heat source and explore implications for neutron star structure.

Main Methods:

  • * Employed detailed nuclear reaction network calculations for heating and cooling.
  • * Utilized realistic nuclear compositions for neutron star crust modeling.
  • * Analyzed X-ray observations of KS 1731-260's cooling behavior in quiescence.

Main Results:

  • * The required strength of the shallow heat source in KS 1731-260 was reduced by over a factor of 3.
  • * This reduction (a 5σ difference) alleviates the need for exotic physics.
  • * Evidence suggests an impure nuclear pasta layer in the inner crust of KS 1731-260.
  • * Constraints were obtained on the surface burning modes of KS 1731-260.

Conclusions:

  • * The shallow heat source in accreting neutron stars like KS 1731-260 is less intense than previously assumed.
  • * The findings support more conventional explanations for neutron star crustal heating.
  • * The potential presence of nuclear pasta warrants further observational and theoretical investigation.