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Neutrino emissivity, strong magnetic fields and cooling of neutron stars
Author(s) -
Coelho E. L.,
Chiapparini M.,
Bracco M. E.,
Negreiros R. P.
Publication year - 2014
Publication title -
astronomische nachrichten
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.394
H-Index - 63
eISSN - 1521-3994
pISSN - 0004-6337
DOI - 10.1002/asna.201412084
Subject(s) - neutron star , physics , neutrino , pulsar , emissivity , magnetic field , astrophysics , stars , nuclear physics , optics , quantum mechanics
Abstract The direct Urca process is an extremely efficient mechanism for cooling a proto neutron star after its formation. It is believed to be the process responsible for the cooling of proto‐neutron stars after the first 100 years of life. One of the most interesting kind of neutron stars are the pulsars, which are highly magnetized neutron stars with fields up to 10 14 G at the surface. In this work we investigate the influence of strong magnetic fields on the cooling of pulsars due to the neutrino emissivity coming from the direct Urca process. The matter is described using a relativistic mean‐field model at zero temperature. We calculate numerically the emissivity of neutrinos for different magnetic fields as a function of the baryon density and compare the results for the case without a magnetic field. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)