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MHD Simulations of Disk-Magnetized Star Interactions in Quiescent Regime: Funnel Flows and Angular Momentum Transport

M. M. Romanova·G. V. Ustyugova·A. V. Koldoba·R. V. E. Lovelace
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Abstract

Magnetohydrodynamic (MHD) simulations have been used to study disk accretion to a rotating magnetized star with an aligned dipole moment. Quiescent initial conditions were developed in order to avoid the fast initial evolution seen in earlier studies. A set of simulations was performed for different stellar magnetic moments and rotation rates. Simulations have shown that the disk structure is significantly changed insidea radius r_{br} where magnetic braking is significant. In this region the disk is strongly inhomogeneous. Radial accretion of matter slows as it approaches the area of strong magnetic field and a dense ring and funnel flow form at the magnetospheric radius r_m where the magnetic pressure is equal to the total, kinetic plus thermal, pressure of the matter.

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M. M. Romanova, G. V. Ustyugova, A. V. Koldoba, R. V. E. Lovelace. 2002-09-20. MHD Simulations of Disk-Magnetized Star Interactions in Quiescent Regime: Funnel Flows and Angular Momentum Transport. https://doi.org/10.1086/342464

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