Effect of weak interaction on kaon condensation and cooling of neutron stars.

Details Effect of weak interaction on kaon condensation and cooling of neutron stars. Effect of weak interaction on kaon condensation and cooling of neutron stars.

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994nupha.571..758f&link_type=abstract

Nuclear Physics A, Vol. 571, No. 4, p. 758 - 783

Physics

Nuclear Physics

31

Neutron Stars: Cooling

Scientific paper

Kaon condensation and its implication in the cooling mechanism in neutron stars are investigated within a framework of current algebra and PCAC. The weak interaction, nýp+K-, is shown to play a significant role in determining not only the critical density but also the equation of state of the K- condensed phase. The chemical equilibrium for the weak interaction leads to large proton-admixture. In connection with this result, the possibility of the direct URCA process, n→p+e-+ν¯e, p+e-→n+νe, is investigted. It is shown that, within a simple treatment without the nuclear interactions such as the symmetry energy, the kinematical condition for the direct URCA process is not satified despite the large proton-mixing, due to the resulting small electron Fermi momentum. The physical content of the K- condensation from a viewpoint of strangeness degrees of freedom is also discussed.

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