Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...456..696l&link_type=abstract
Astrophysical Journal v.456, p.696
Astronomy and Astrophysics
Astronomy
22
Accretion, Accretion Disks, Magnetohydrodynamics: Mhd, Stars: Pre-Main-Sequence
Scientific paper
In earlier models of magnetic interaction between a central T Tauri star and its associated disk, a stellar corotating magnetosphere was assumed, and consequently a large vertical angular velocity shear exists between the disk surface and the magnetosphere. The evaluated magnetic torque on the star is then dependent on the macroresistivity of the disk, regardless of true nature of the accretion flow. However, we may argue that a corotating magnetosphere with an enormous rotational shearing placed on the disk surface does not exist in reality, and the stellar magnetic fields are anchored to the disk non-slippage assumption. Hence the disk-star system may undergo a dynamical coupling in which a field-aligned plasma motion, via either the accretion flow or a disk wind, removes a local winding of the magnetic fields. As a result, the accretion flow and the magnetic torque are closely related through MHD equations. We calculated the angular momentum accretion rate in our model with parameters typically for classic T Tauri stars (CTTSs) and found that it is about one order of magnitude smaller than that of a hydrodynamical accretion, indicating that most of the angular momentum of the accretion flow goes to the disk (but not to the star). The result may lead to the conclusion that the magnetized accretion of angular momentum onto the central CTTS can be quite inefficient. This may naturally explain why CTTSs rotate more slowly than T Tauri stars without disks. The model predicts that if the outer radius of the magnetosphere is large the central star is in a rotational equilibrium at rin ≃ 0.7rco, where rin and rco are the inner disk and the corotation radii.
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