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Neutron star evolutionary sequencesDetailed 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.
Document ID
19820047371
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Richardson, M. B.
(New York, State University Albany; Rochester, University, Rochester, NY; Illinois, University, Urbana, IL, United States)
Van Horn, H. M.
(Rochester, University Rochester, NY, United States)
Ratcliff, K. F.
(New York, State University Albany, NY, United States)
Malone, R. C.
(Cornell University Ithaca, NY; Los Alamos National Laboratory, Los Alamos, NM, United States)
Date Acquired
August 10, 2013
Publication Date
April 15, 1982
Publication Information
Publication: Astrophysical Journal
Subject Category
Astrophysics
Accession Number
82A30906
Funding Number(s)
CONTRACT_GRANT: NSF AST-79-09391
CONTRACT_GRANT: NSG-7653
Distribution Limits
Public
Copyright
Other

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