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

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.

22 figures, to appear in ApJ, 10 October, 2002

References in corpus (1)

• Poynting Jets from Accretion Disks

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