Electrical conductivity of neutron star cores in the presence of a magnetic field |
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Authors: | D G Yakovlev D A Shalybkov |
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Institution: | (1) A. F. Ioffe Institute of Physics and Technology, Leningrad, U.S.S.R. |
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Abstract: | General theory of electrical conductivity of a multicomponent mixture of degenerate fermions in a magnetic fieldB, developed in the preceding article (this volume), is applied to a matter in neutron star interiors at densities ![rgr](/content/j293316611312113/xxlarge961.gif) ![gap](/content/j293316611312113/xxlarge8819.gif) 0, where 0 = 2.8×1014 g cm–3 is the standard nuclear matter density. A model of free-particle mixture ofn, p, e is used, with account for appearance of –-hyperons at >
c
, where
c
4 0. The electric resistivities along and acrossB, ![Rscr](/content/j293316611312113/xxlarge8475.gif) and ![Rscr](/content/j293316611312113/xxlarge8475.gif) , and the Hall resistivity
H
are calculated and fitted by simple analytical formulae at ![rgr](/content/j293316611312113/xxlarge961.gif) ![le](/content/j293316611312113/xxlarge8804.gif)
c
and >
c
for the cases of normal or superfluid neutrons provided other particles are normal. Charge transport alongB is produced by electrons, due to their Coulombic collisions with other charged particles; ![Rscr](/content/j293316611312113/xxlarge8475.gif) is independent ofB and almost independent of the neutron superfluidity. Charge transport acrossB at largeB may be essentially determined by other charged particles. If ![rgr](/content/j293316611312113/xxlarge961.gif) ![le](/content/j293316611312113/xxlarge8804.gif)
c
, one has ![Rscr](/content/j293316611312113/xxlarge8475.gif) = ![Rscr](/content/j293316611312113/xxlarge8475.gif) 1 + (B/B
0)2] for the normal neutrons, and ![Rscr](/content/j293316611312113/xxlarge8475.gif) for the superfluid neutrons, while
H
= ![Rscr](/content/j293316611312113/xxlarge8475.gif)
B/B
e
for both cases. HereB
e
109
T
8
2
G,B
0 1011
T
8
2
G, andT
8 is temperature in units of 108 K. Accordingly for the normal neutrons atB B
0, the transverse resistivity ![Rscr](/content/j293316611312113/xxlarge8475.gif) suffers an enhancement, 1/4 1. When ![rgr](/content/j293316611312113/xxlarge961.gif) 5 0 andB varies from 0 toB B
p
1013
T
8
2
G, ![Rscr](/content/j293316611312113/xxlarge8475.gif) increases by a factor of about 103–104 and
H
changes sign. WhenB B
p
, ![Rscr](/content/j293316611312113/xxlarge8475.gif) remains constant for the superfluid neutrons, and
H
B
2 for the normal neutrons, while
H
B for any neutron state. Strong dependence of resistivity onB, T, and may affect evolution of magnetic fields in neutron star cores. In particular, the enhancement of ![Rscr](/content/j293316611312113/xxlarge8475.gif) at highB may noticeably speed up the Ohmic decay of those electric currents which are perpendicular toB. |
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Keywords: | |
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