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Three-dimensional Simulations of Disk Accretion to an Inclined Dipole. I. Magnetospheric Flows at Different Θ, 2003

By M. M. Romanova, G. V. Ustyugova, A. V. Koldoba, J. V. Wick and R. V. E. Lovelace

Abstract

stars Draft version February 2, 2008 We present results of fully three-dimensional magnetohydrodynamic (MHD) simulations of disk accretion to a slowly rotating magnetized star with its dipole moment inclined at an angle Θ to the rotation axis of the disk (which is assumed to be aligned with the spin axis of the star). The main goal was to investigate the pattern of magnetospheric flow and the disk-star interaction for a variety of inclination angles Θ. We observed that at Θ = 0 ◦ , the disk stops at magnetospheric radius rm, and matter flows to the star through axisymmetric funnel flows, as observed in earlier axisymmetric simulations. However, when the dipole moment of the star is inclined, then the flow becomes non-axisymmetric. The non-axisymmetry becomes notable at very small inclination angles Θ ∼ 2 ◦ − 5 ◦. The pattern of magnetospheric flow is different at different Θ. For relatively small angles, Θ ∼ < 30 ◦ , the densest matter flows to the star mostly in two streams, which follow paths to the closest magnetic pole. The streams typically co-rotate with the star, but they may precess about the star for Θ < 10 ◦. At intermediate angles, 30 ◦

Year: 2013
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