Effects of Magnetized Winds on Advective Disks. I. A Self-similar Solution

Details Effects of Magnetized Winds on Advective Disks. I. A Self-similar Solution Effects of Magnetized Winds on Advective Disks. I. A Self-similar Solution

Oct 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...487..769s&link_type=abstract

Astrophysical Journal v.487, p.769

Physics

3

Accretion, Accretion Disks, Black Hole Physics, Magnetic Fields, Magnetohydrodynamics: Mhd

Scientific paper

In this paper we investigate the effects of a large-scale magnetic field (with open field lines) on the structure of an advective accretion disk. We find self-similar solutions to the MHD equations describing the disk/magnetic field system; these equations reduce to the case studied by Narayan & Yi (1994) in the absence of an external, macroscopic magnetic field. Our main assumptions are the existence of a hot, tenuous corona above and below the disk, and the presence of a wind starting from the base of the corona and centrifugally accelerated along the field lines up to the Alfven surface. The wind appears to be the most efficient mechanism for extracting angular momentum from the inflowing gas, even when the mass lost in the wind is negligible with respect to the mass accreted; other notable effects of the interplay between the disk structure and the magnetic field with its associated wind include a bending of the field lines toward the surface of the disk (dragging of the field by the accreting matter), a squeezing effect (the disk scale height is reduced because of a magnetic pressure gradient), an increased radial infall velocity (consequence of the quicker loss of angular momentum), and a decrease of the gas temperature in the disk. We can equivalently describe the loss of angular momentum in the wind by introducing an effective viscosity parameter alpha eff, which can become greater than 1 regardless of the true viscosity parameter alpha .

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