The radial disc structure around a magnetic neutron star: analytic and semi-analytic solutions

Details The radial disc structure around a magnetic neutron star: analytic and semi-analytic solutions The radial disc structure around a magnetic neutron star: analytic and semi-analytic solutions

Jul 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.298..223b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 298, Issue 1, pp. 223-230.

Astronomy and Astrophysics

Astronomy

12

Accretion, Accretion Discs, Magnetic Fields, Stars: Neutron

Scientific paper

The radial structure of a thin accretion disc is calculated in the presence of a central dipole magnetic field aligned with the rotation axis. The problem is treated using a modified expression for the turbulent magnetic diffusion, which allows the angular momentum equation to be integrated analytically. The governing algebraic equations are solved iteratively between 1 and 10^4 stellar radii. An analytic approximation is provided that is valid near the disruption radius at about 100 stellar radii. At that point, which is approximately 60 per cent of the Alfven radius and typically about 30 per cent of the corotation radius, the disc becomes viscously unstable. This instability results from the fact that both radiation pressure and opacity caused by electron scattering become important. This in turn is a consequence of the magnetic field which leads to an enhanced temperature in the inner parts. This is because the magnetic field gives rise to a strongly enhanced vertically integrated viscosity, so that the viscous torque can balance the magnetic torque.

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