Unstable Disk Accretion onto Magnetized Stars: First Global Three-dimensional Magnetohydrodynamic Simulations

Details Unstable Disk Accretion onto Magnetized Stars: First Global Three-dimensional Magnetohydrodynamic Simulations Unstable Disk Accretion onto Magnetized Stars: First Global Three-dimensional Magnetohydrodynamic Simulations

Feb 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...673l.171r&link_type=abstract

The Astrophysical Journal, Volume 673, Issue 2, pp. L171-L174.

Astronomy and Astrophysics

Astronomy

47

Accretion, Accretion Disks, Instabilities, Magnetohydrodynamics: Mhd, Stars: Magnetic Fields

Scientific paper

We report on the first global three-dimensional (3D) MHD simulations of disk accretion onto a rotating magnetized star through the Rayleigh-Taylor instability. The star has a dipole field misaligned relative to the rotation axis by a small angle Θ. Simulations show that, depending on the accretion rate, a star may be in the stable or unstable regime of accretion. In the unstable regime, matter penetrates deep into the magnetosphere through several elongated ``tongues'' which deposit matter at random places on the surface of the star, leading to stochastic light curves. In the stable regime, matter accretes in ordered funnel streams and the light curves are almost periodic. A star may switch between these two regimes depending on the accretion rate and may thus show alternate episodes of ordered pulsations and stochastic light curves. In the intermediate regime, both stochastic and ordered pulsations are observed. For Θ>30deg, the instability is suppressed and stable accretion through funnel streams dominates.

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