Magnetic field stability of neutron stars

Details Magnetic field stability of neutron stars Magnetic field stability of neutron stars

Jan 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...324..966w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 324, Jan. 15, 1988, p. 966-973.

Astronomy and Astrophysics

Astrophysics

10

Interstellar Magnetic Fields, Magnetic Stars, Neutron Stars, Stellar Rotation, White Dwarf Stars, X Ray Binaries, Gamma Ray Bursts, Perturbation Theory, Time Dependence

Scientific paper

The authors show that a purely poloidal field in the superconducting core of a neutron star is secularly unstable over the ohmic dissipation time scale of the crusts. Very old neutron stars may thus have strong but disordered surface fields. For rotating stars, solutions are derived for the fluid interior which illustrate how the inertial forces in the rotating frame are absorbed by pressure and field perturbations as the instability progresses.

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