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J. Raymond (CfA)
Accretion disks transport angular momentum and generate heat by a mechanism formerly known as `viscosity' and now known as the Magnetorotational Instability. To the extent that it occurs below the disk photosphere, it is difficult to learn much about the process observationally except perhaps from flickering time scales. A substantial fraction of the energy is expected to emerge through the disk photosphere, however, producing coronae and winds. This talk describes constraints on accretion disk coronae produced by photoionization, thermal conduction or magnetic heating. This work is supported by NASA Grant NAG5-10353 and CHANDRA grant GO2-3032X.
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Bulletin of the American Astronomical Society, 36 #2
© YEAR. The American Astronomical Soceity.