2D and 3D MHD Simulations of Disk Accretion by Rotating Magnetized Stars: Search for Variability
arXiv:astro-ph/0604116 · doi:10.1016/j.asr.2006.04.019
Abstract
We performed 2D and full 3D magnetohydrodynamic simulations of disk accretion to a rotating star with an aligned or misaligned dipole magnetic field. We investigated the rotational equilibrium state and derived from simulations the ratio between two main frequencies: the spin frequency of the star and the orbital frequency at the inner radius of the disk. In 3D simulations we observed different features related to the non-axisymmetry of the magnetospheric flow. These features may be responsible for high-frequency quasi-periodic oscillations (QPOs). Variability at much lower frequencies may be connected with restructuring of the magnetic flux threading the inner regions of the disk. Such variability is specifically strong at the propeller stage of evolution.
11 pages, 11 figures, invited review presented at COSPAR Colloquium "Spectra & Timing of Compact X-ray Binaries", January 17-20, 2005, Mumbai, India. To be published in Advances in Space Research
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- Wave Excitation in Disks Around Rotating Magnetic Stars
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