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We report on the first global three-dimensional (3D) MHD simulations of diskaccretion onto a rotating magnetized star through the Rayleigh-Taylorinstability. The star has a dipole field misaligned relative to the rotationaxis by a small angle Theta. Simulations show that, depending on the accretionrate, a star may be in the stable or unstable regime of accretion. In theunstable regime, matter penetrates deep into the magnetosphere through severalelongated "tongues" which deposit matter at random places on the surface of thestar, leading to stochastic light-curves. In the stable regime, matter accretesin ordered funnel streams and the light-curves are almost periodic. A star mayswitch between these two regimes depending on the accretion rate and may thusshow alternate episodes of ordered pulsations and stochastic light-curves. Inthe intermediate regime, both stochastic and ordered pulsations are observed.For Theta > 30 degrees, the instability is suppressed and stable accretionthrough funnel streams dominates.

Unstable Disk Accretion to Magnetized Stars: First Global 3D MHD Simulations