Disc structure around strongly magnetic accretors: a full disc solution with buoyancy diffusivity

Details Disc structure around strongly magnetic accretors: a full disc solution with buoyancy diffusivity Disc structure around strongly magnetic accretors: a full disc solution with buoyancy diffusivity

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.301..558c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 301, Issue 2, pp. 558-568.

Astronomy and Astrophysics

Astronomy

10

Accretion, Accretion Discs, Diffusion, Magnetic Fields, Stars: Magnetic Fields, Stars: Neutron

Scientific paper

A full numerical solution is found for the effect of a strongly magnetic star on its accretion disc, for the case of magnetic buoyancy diffusion. As in the previously considered case of turbulent diffusion, the disc becomes disrupted when magnetic and viscous stresses become comparable. A magnetically induced temperature elevation leads to electron scattering opacity and radiation pressure becoming significant far from the stellar surface, with consequent viscous instability and vertical disruption of the disc. This, together with the previous turbulent case, suggests that such a disruption mechanism owing to strongly magnetic accretors is generally operable.

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