Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991ap%26ss.176..191y&link_type=abstract
Astrophysics and Space Science, Volume 176, Issue 2, pp.191-215
Astronomy and Astrophysics
Astrophysics
27
Scientific paper
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 ρ≳ρ0, where ρ0 = 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 ρ>ρ c , where ρ c ≈4ρ0. The electric resistivities along and acrossB, ℛ∥ and ℛ⊥, and the Hall resistivity ℛ H are calculated and fitted by simple analytical formulae at ρ≤ρ c and ρ>ρ 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; ℛ∥ is independent ofB and almost independent of the neutron superfluidity. Charge transport acrossB at largeB may be essentially determined by other charged particles. If ρ≤ρ c , one has ℛ⊥ = ℛ∥[1 + (B/B 0)2] for the normal neutrons, and ℛ∥ for the superfluid neutrons, while ℛ H = ℛ∥ 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 ℛ∥ suffers an enhancement, ℛ1/4 ≪ ℛ1. When ρ≳5ρ0 andB varies from 0 toB˜B p ∞ 1013 T {8/2}G, ℛ⊥ increases by a factor of about 103 104 and ℛ H changes sign. WhenB≫B p , ℛ⊥ remains constant for the superfluid neutrons, and ℛ H ∞B 2 for the normal neutrons, while ℛ H ∞B for any neutron state. Strong dependence of resistivity onB, T, and ρ may affect evolution of magnetic fields in neutron star cores. In particular, the enhancement of ℛ⊥ at highB may noticeably speed up the Ohmic decay of those electric currents which are perpendicular toB.
Shalybkov Dmitry A.
Yakovlev Dmitry G.
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