The steady-state structure of accretion discs in central magnetic fields

Abstract

We develop a new analytic solution for the steady-state structure of a thin accretion disc under the influence of a magnetic field that is anchored to the central star. The solution takes a form similar to that of Shakura and Sunyaev and tends to their solution as the magnetic moment of the star tends to zero. As well as the Kramer's law case, we obtain a solution for a general opacity. The effects of varying the mass transfer rate, spin period and magnetic field of the star as well as the opacity model applied to the disc are explored for a range of objects. The solution depends on the position of the magnetic truncation radius. We propose a new approach for the identification of the truncation radius and present an analytic expression for its position.

11 pages, 7 figures, accepted by MNRAS

References in corpus (8)

• Using FU Orionis Outbursts to Constrain Self-Regulated Protostellar Disk Models
• Rosseland and Planck Mean Opacities for Protoplanetary Discs
• Magnetic braking of T Tauri stars
• AE Aquarii: how CVs descend from supersoft binaries
• MHD Simulations of Bondi Accretion to a Star in the "Propeller" Regime
• Accretion Disc Evolution in Single and Binary T Tauri Stars
• The behaviour of quiescent accretion discs in dwarf novae
• Outbursts of Young Stellar Objects

Cited by in corpus (5)

• Magnetically Torqued Thin Accretion Disks
• Magnetically moderated outbursts of WZ Sagittae
• The role of Hall diffusion in the magnetically threaded thin accretion discs
• Thin accretion disc with a corona in a central magnetic field
• Effects of magnetic field on the radiation pressure dominated discs around neutron stars