Cooling of neutron stars

Details Cooling of neutron stars Cooling of neutron stars

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992rvmp...64.1133p&link_type=abstract

Reviews of Modern Physics (ISSN 0034-6861), vol. 64, no. 4, p. 1133-1140.

Physics

142

Neutron Stars, Stellar Interiors, Stellar Radiation, Stellar Temperature, Cooling, Neutrinos, Nucleons, Stellar Evolution

Scientific paper

It is at present impossible to predict the interior constitution of neutron stars based on theory and results from laboratory studies. It has been proposed that it is possible to obtain information on neutron star interiors by studying thermal radiation from their surfaces, because neutrino emission rates, and hence the temperature of the central part of a neutron star, depend on the properties of dense matter. The theory predicts that neutron stars cool relatively slowly if their cores are made up of nucleons, and cool faster if the matter is in an exotic state, such as a pion condensate, a kaon condensate, or quark matter. This view has recently been questioned by the discovery of a number of other processes that could lead to copious neutrino emission and rapid cooling.

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