Alfvénic Heating of Accretion Disks

Details Alfvénic Heating of Accretion Disks Alfvénic Heating of Accretion Disks

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000rmxac...9..103v&link_type=abstract

"Astrophysical Plasmas: Codes, Models, and Observations, Proceedings of the conference held in Mexico City, October 25-29, 1999,

Astronomy and Astrophysics

Astrophysics

Scientific paper

In this work, we investigate the effects of heating generated by nonlinear and turbulent damping of Alfvén waves. Our results are a function of two parameters: f=δ v/vA, which is a measure of the degree of turbulence, and F = ϖ/Ωi, which is the average frequency of the waves (δ v, vA and ϖ are the amplitude, velocity and frequency of the Alfvén waves, respectively, and Ωi is the ion cyclotron frequency). Only a small portion of the disk is studied, ranging from 0.1 AU to 1.4 AU. We find that, when compared with the heating generated by viscous dissipation, the Alfvénic heating is important for R > 0.5 AU. An increase in temperature occurs, which causes an increase in the degree of ionization of the system. When irradiation from the central star is taken into account the increase in temperature is much more significant. Due to Alfvénic heating, the influence of the magnetorotational instability extends to a greater part of the protostellar accretion disk.

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