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Neutron Star Cooling: Effects of Envelope Physics

Published online by Cambridge University Press:  04 August 2017

Kenneth A. Van Riper
Kenneth A. Van Riper*
Affiliation:
Computational Physics Group, Applied Theoretical Physics Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA

Abstract

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Neutron star cooling calculations are reported which employ improved physics in the calculation of the temperature drop through the atmosphere. The atmosphere microphysics is discussed briefly. The predicted neutron star surface temperatures, in the interesting interval 300 ≤ t (yr) ≤ 105, do not differ appreciably from the earlier results of Van Riper and Lamb (1981) for a non-magnetic star; for a magnetic star, the surface temperature is lower than in the previous work. Comparison with observational limits show that an exotic cooling mechanism such as neutrino emission from a pion-condensate or in the presence of percolating quarks, is not required, unless the existence of a neutron star in the Tycho or SN1006 supernova remnants is established.

Type
V. Compact Objects Associated With Supernova Remnants, Pulsars and Neutron Stars
Information
Symposium - International Astronomical Union , Volume 101: Supernova Remnants and Their X-Ray Emission , 1983 , pp. 513 - 516
Copyright
Copyright © Reidel 1983 

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