Physics
Scientific paper
May 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aps..may.k1403k&link_type=abstract
American Physical Society, APS/AAPT Joint Meeting, May 2-5, 1996, abstract #K14.03
Physics
Scientific paper
One of the key unsolved problems in the theory of accretion disks is the nature of the angular momentum transport mechanism. In one attractive class of models, which may apply, in particular, to disks in active galactic nuclei (AGNs) and around young stellar objects (YSOs), this transport is attributed to centrifugally driven winds that are launched magnetically from the disk surfaces. In this scenario, the disk is threaded by open magnetic field lines, and the magnetic torque associated with this large-scale field removes the angular momentum of the accreted matter and transfers it to the outflowing gas. The wind is powered by the liberated gravitational potential energy and can in principle transport a large fraction of that energy in the form of a Poynting flux. This mechanism leads to a natural interpretation of the bipolar outflows and jets that are commonly observed in AGNs and YSOs. I present recent results on quasi-steady models of accretion disks of this type and illustrate some of the observational consequences of disk-driven hydromagnetic winds. In particular, I show that, because of their unique kinematic and thermal structure, such outflows might account for some of the defining properties of AGNs and YSOs.
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