Force-free magnetic fields in the fluid interiors of neutron stars

Easson, I.

doi:10.1038/263486a0

Nature

1976

DOI: 10.1038/263486a0

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Force-free magnetic fields in the fluid interiors of neutron stars

I. Easson

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Cited by 4 publications

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Some problems of pulsar physics or I'm madly in love with electricity

Arons

1979

Space Sci Rev

181

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Some current topics in the theory of pulsar magnetospheres and their emission are reviewed. The mode of plasma supply and its consequences for structure of planetary and stellar magnetospheres is discussed. In the pulsar case, the plasma is supplied by electrical forces, in contrast to all other known examples. The resulting theories of particle acceleration along polar field lines are then reviewed, and the total energization of the charge separated plasma is summarized, when pair creation is absent. The effects of pair creation are reviewed using models of the resulting steady and unsteady flows, when the polar zones of the pulsar emit either electrons or ions. The application of these theories of acceleration and plasma supply to pulsars is discussed, with particular attention paid to the total amount of electron-positron plasma created and its momentum distribution. Qualitative agreement is shown between the spatial structure of the relativistically outflowing plasma described in one version of these models and the morphology of pulsar wave forms. Various aspects of radiation emission and transport are summarized, based on the polar current flow model with pair creation, and the phenomenon of marching subpulses is discussed. The corotation beaming and the relativistically expanding current sheet models for pulsar emission are also discussed briefly, and the paper concludes with a brief discussion of the relation between the theories of polar flow with pair plasma and the problem of the energization of the Crab Nebula.

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Some problems of pulsar physics or I'm madly in love with electricity

Arons

1979

Space Sci Rev

181

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Dissipation by thermal forces in quantum plasmas

Burman

McClelland

1984

J. Plasma Phys.

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This paper deals with degenerate Fermi–Dirac plasmas in which transport is by quasi-particles that form a dilute gas described by the Boltzmann equation. The off-equilibrium part of the distribution function of each species is estimated by expanding it in terms of the fluid velocity of the species, relative to the plasma, and its relative heat flux vector. Expressions for the frictional forces acting between the species, consisting of a relaxation-model force and a thermal force, are obtained. These are used in a plasma dissipation formalism, yielding, for ternary partially ionized plasmas, a generalized Ohm law and an ambipolar diffusion law. The results are applied to neutron star matter, consisting of thermally ultra-relativistic electrons and non-relativistic protons and neutrons, with the mass density dominated by the neutrons. The dissipation formalism is used to obtain an expression for the magnetic force on this material.

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Interior magnetohydrodynamic structure of a rotating relativistic star

Bekenstein

Oron

1979

Phys. Rev. D

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We study the interior magnetohydrodynamic structure of a rotating stationary axisymmetric neutron star. We assume the fluid is ideal, infinitely conducting, and flows only azimuthaly. We justify this assumption by considering in detail the superfluid physics in the interior. We obtain some of our results by taking a certain limit of previously discovered magnetohydrodynamic conservation laws. We show that the angular velocity, electric and magnetic potentials, and the red-shifted chemical potential are constant on magnetic surfaces. We demonstrate that the absence of meridional circulation implies the vanishing of the toriodal magnetic field. This clashes with previous arguments from the probable evolution of the magnetic field during the collapse to the neutron star. We solve completely Maxwell's equations for the distribution of magnetic field strength, and we show that the magnetic surfaces are the equipotentials of a simple geometrical invariant. With neglect of gravitational effects the magnetic field must be uniform in the interior in accordance with the Deutsch model, but at variance with numerous other models which have been proposed for ordinary stars. Gravitation causes the magnetic surfaces to flare out toward the polar regions and enhances the central field as compared to the polar field. The star must be charged; the charge distribution depends on the magnetic field strength and on the angular velocity relative to the local inertial frames.

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Force-free magnetic fields in the fluid interiors of neutron stars

Cited by 4 publications

References 3 publications

Some problems of pulsar physics or I'm madly in love with electricity

Some problems of pulsar physics or I'm madly in love with electricity

Dissipation by thermal forces in quantum plasmas

Interior magnetohydrodynamic structure of a rotating relativistic star

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