Neutron star evolutionary sequences

Abstract

view Abstract Citations (81) References (73) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Neutron star evolutionary sequences. Richardson, M. B. ; van Horn, H. M. ; Ratcliff, K. F. ; Malone, R. C. Abstract Detailed numerical calculations which are solutions of the full set of general relativistic equations describing the evolution of a spherical star are presented, for the case of the evolution of neutron stars that are cooling over the central temperatures range of 10 to the 10th to 10 to the 7th K. The effects of nucleon superfluidity in the inner crust and core are included, and models are constructed with and without a pion condensate at high densities. It is found that the localized neutrino cooling which dominates the early evolution of neutron stars is so rapid that heat transport within the star cannot keep pace, and temperature distribution is not isothermal. The residual contraction of the neutron star during the early cooling phase contributes little to the heat budget of the star, and most of the gravitational energy released raises the Fermi energy of the degenerate nucleons. It is concluded that since calculations with and without pion condensate are consistent with the upper limits of current observations, these are not sufficient in distinguishing between the various models of neutron star cooling. Publication: The Astrophysical Journal Pub Date: April 1982 DOI: 10.1086/159865 Bibcode: 1982ApJ...255..624R Keywords: Neutrinos; Neutron Stars; Particle Emission; Stellar Evolution; Stellar Temperature; Thermal Radiation; Equations Of State; Pions; Relativistic Effects; Stellar Models; Stellar Radiation; Surface Temperature; Astrophysics full text sources ADS | data products SIMBAD (2)