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Title: Magnetohydrodynamics of neutron star interiors

Abstract

Magnetohydrodynamic equations for the charged particles in the fluid interior of a neutron star are derived from the Landau-Boltzmann kinetic equations. It is assumed that the protons are normal and the neutrons are superfluid. The dissipative processes associated with the weak interactions are shown to be negligible except in very hot neutron stars; we neglect them here. Among the topics discussed are: the influence of the neutron-proton nuclear force (Fermi liquid corrections) on the magnetohydrodynamics; the effects of the magnetic field on the pressure, viscosity, and heat conductivity tensors; the plasma equation of state; and the form of the generalized Ohm's law.

Authors:
;
Publication Date:
Research Org.:
Department of Physics, University of Illinois at Urbana-Champaign
OSTI Identifier:
6272256
Resource Type:
Journal Article
Journal Name:
Astrophys. J.; (United States)
Additional Journal Information:
Journal Volume: 227:3
Country of Publication:
United States
Language:
English
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; NEUTRON STARS; MAGNETOHYDRODYNAMICS; STAR MODELS; CHARGED PARTICLES; ENTROPY; EQUATIONS OF STATE; HYDRODYNAMICS; MAGNETIC FIELDS; OHM LAW; QUANTUM PLASMA; SUPERFLUIDITY; THERMAL CONDUCTIVITY; VISCOSITY; EQUATIONS; FLUID MECHANICS; MATHEMATICAL MODELS; MECHANICS; PHYSICAL PROPERTIES; PLASMA; STARS; THERMODYNAMIC PROPERTIES; 640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources

Citation Formats

Easson, I., and Pethick, C.J. Magnetohydrodynamics of neutron star interiors. United States: N. p., 1979. Web. doi:10.1086/156808.
Easson, I., & Pethick, C.J. Magnetohydrodynamics of neutron star interiors. United States. doi:10.1086/156808.
Easson, I., and Pethick, C.J. Thu . "Magnetohydrodynamics of neutron star interiors". United States. doi:10.1086/156808.
@article{osti_6272256,
title = {Magnetohydrodynamics of neutron star interiors},
author = {Easson, I. and Pethick, C.J.},
abstractNote = {Magnetohydrodynamic equations for the charged particles in the fluid interior of a neutron star are derived from the Landau-Boltzmann kinetic equations. It is assumed that the protons are normal and the neutrons are superfluid. The dissipative processes associated with the weak interactions are shown to be negligible except in very hot neutron stars; we neglect them here. Among the topics discussed are: the influence of the neutron-proton nuclear force (Fermi liquid corrections) on the magnetohydrodynamics; the effects of the magnetic field on the pressure, viscosity, and heat conductivity tensors; the plasma equation of state; and the form of the generalized Ohm's law.},
doi = {10.1086/156808},
journal = {Astrophys. J.; (United States)},
number = ,
volume = 227:3,
place = {United States},
year = {1979},
month = {2}
}