Crystalline nuclei and the Pomeranchuk effect in neutron stars

Abstract

The transition from the liquid to the crystalline phase upon adiabatic compression of the core of a neutron star during its ''birth'' leads to a sharp cooling of the crystalline neutron core. A similar problem was considered previously for liquid He/sup 3/ by I. Ya. Pomeranchuk. The effect strongly influences the character of neutron star cooling curves. Upon further evolution of the star either fusion of the crystalline nucleus or further crystallization of the neutron liquid is possible. In both cases radial stresses develop in the star, as a consequence of which ''starquakes'' are possible.