Thermal evolution of neutron stars and constraints on their internal properties

Details Thermal evolution of neutron stars and constraints on their internal properties Thermal evolution of neutron stars and constraints on their internal properties

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011sf2a.conf..573f&link_type=abstract

SF2A-2011: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: G. Alecian, K. Belkacem,

Astronomy and Astrophysics

Astrophysics

Neutron Stars, Cooling, Dense Matter, Equation Of State, Superfluidity

Scientific paper

Neutron stars, the end point of the life of massive stars, are cosmic laboratories for various fields of physics, in particular for nuclear physics of cold and dense matter. The very high densities inside neutron stars can not be reproduced on Earth. Nevertheless, modeling the thermal evolution of both isolated and accreting neutron stars enables to put constraints on the poorly known composition, structure, superfluid and thermal properties of their interior.

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