Abstract
If neutron star interiors are superfluid, heat is dissipated within the star as its rotation is slowed. This process sets a lower limit to the temperature such a star can attain: the limit is such that thermal X-ray emission from certain pulsars may be detectable.
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GREENSTEIN, G. Frictional Heating in Neutron Stars. Nature Physical Science 232, 117–119 (1971). https://doi.org/10.1038/physci232117a0
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DOI: https://doi.org/10.1038/physci232117a0
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