The cooling of neutron stars

Details The cooling of neutron stars The cooling of neutron stars

Mar 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980jphys..41c.139s&link_type=abstract

(Centre National de la Recherche Scientifique, Colloque International sur la Physique de la Matiere Dense, Paris, France, Sept.

Astronomy and Astrophysics

Astronomy

Cooling, Hot Stars, Neutron Stars, Supernova Remnants, Energy Dissipation, Stellar Interiors, Stellar Luminosity, Stellar Temperature, Surface Temperature, X Ray Astronomy

Scientific paper

Our present understanding of the cooling of hot neutron stars formed in supernovae collapses is briefly reviewed. The neutrino energy loss dominant in the early stages of the cooling is discussed for an equation of state involving only nucleon degrees of freedom and in the presence of a pion condensate. Assuming that the collapse of supernovae always produces hot neutron stars, it is shown that recent results from X-ray observations of young supernovae remnants by the Einstein Observatory are suggestive of the presence of pion condensates in the interior of neutron stars.

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