MHD simulations of the magnetic coupling between a young star and its accretion disk

Details MHD simulations of the magnetic coupling between a young star and its accretion disk MHD simulations of the magnetic coupling between a young star and its accretion disk

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sf2a.conf..447b&link_type=abstract

SF2A-2006: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: D. Barret, F. Casoli, G.

Astronomy and Astrophysics

Astrophysics

Scientific paper

The magnetic star-disk interaction is important in the context of the dynamic evolution of low mass protostars. In particular, Classical T-Tauri Stars (CTTS) have a puzzling low rotation rate despite accretion. In such a complex star-disk system, we need to take into account the stellar and disk magnetic fields with a realistic accretion disk structure. Magnetohydrodynamic (MHD) simulations are necessary to support and extend analytical work. First, we briefly review theoretical models and past numerical work. We discuss the difficulties to set up initial conditions with a realistic accretion disk structure, as well as the choice of the boundary conditions at the star surface to correctly handle angular momentum transport. Then, we present our 2.5D MHD simulations done with the Versatile Advection Code (VAC), modified here to handle strong dipole stellar fields by a splitting strategy for the magnetic field. In this paper, we only consider the stellar magnetic field and its interaction with the disk. We confirm the process of poloidal magnetic field expansion when the disk resistivity is negligible, and identify physical conditions needed for the formation of accretion columns.

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