Theory of cooling neutron stars versus observations
D. G. Yakovlev (1,2), O. Y. Gnedin (3), A. D. Kaminker (1), A. Y., Potekhin (1,4) ((1) Ioffe Institute, St. Petersburg; (2) JINA, Notre Dame;, (3) University of Michigan; (4) CRAL, ENS-Lyon)
TL;DR
This paper reviews neutron star cooling theories and discusses how observations of thermal radiation can help constrain the properties of neutron star cores, including the equation of state, neutrino emission, and superfluidity.
Contribution
It provides a comprehensive review of current cooling models and explores their potential to inform about neutron star interior physics through observational data.
Findings
Cooling models can be constrained by thermal radiation observations.
Neutrino emission and superfluid properties significantly affect cooling.
Observations can help determine the neutron star equation of state.
Abstract
We review current state of neutron star cooling theory and discuss the prospects to constrain the equation of state, neutrino emission and superfluid properties of neutron star cores by comparing the cooling theory with observations of thermal radiation from isolated neutron stars.
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