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Thermodynamic Transport Properties in Dense Stars

Published online by Cambridge University Press:  12 April 2016

Terry W. Edwards
Terry W. Edwards*
Affiliation:
Department of Physics and Astronomy, University of Missouri - Columbia

Abstract

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The thermodynamic transport properties of special relativistic imperfect fluids, as found in dense stars, are investigated. These properties, which include thermal and electrical conductivities, electrothermal coefficients, and bulk and shear viscosities may be formulated in terms of the momentum distribution functions obtained from the solution of the Boltzmann transport equation. Spherical harmonic solutions of the relaxation form of the relativistic magnetic Boltzmann transport equation have also been obtained which give the non-equilibrium momentum distribution function perturbation f-f(0) = Δf(p) in terms of electromagnetic and thermal fields.

Type
X. White Dwarf Pulsations
Information
International Astronomical Union Colloquium , Volume 58: Stellar Hydrodynamics , August 1980 , pp. 627 - 633
Copyright
Copyright © Reidel 1980

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