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As a neutron star spins down its core density increases, changing the relative equilibrium concentration and causing deconfinement phase transition as well. Hadron matter is converted into quark matter in the interior, which enhances the deviation of the chemical equilibrium state. We study such deviations and their chemical energy release. Applying our results to the simulation of cooling neutron stars, we find that the surface effective temperature of neutron stars is obviously promoted. This implies that the deconfinement phase transition is able to raise the chemical heating efficiency.

The effect of deconfinement phase transition on rotochemical deviations in stars containing mixed‐phase matter