Mechanical Heating of Protostellar Discs

Details Mechanical Heating of Protostellar Discs Mechanical Heating of Protostellar Discs

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21542920p&link_type=abstract

American Astronomical Society, AAS Meeting #215, #429.20; Bulletin of the American Astronomical Society, Vol. 42, p.353

Astronomy and Astrophysics

Astronomy

Scientific paper

The magnetic field structure of a protostar truncates the accretion disc at some magnetospheric radius greater than the stellar radius. If the stellar rotation axis is not aligned with the disc rotation, then the magnetic stresses at this radius lead to a tilt in the inner disc. The stellar dynamo which produces the field, leads to a varying field and so to a varying tilt. In the right circumstances, such tilting motions can propagate outwards through the disc as warp waves. The waves damp when their frequency matches the local disc Keplerian frequency. If the waves propagate sufficiently far then such wave damping can provide a dominant contribution to local disc heating and so cause local disc flaring. This flaring can in turn cause changes to the disc spectral energy distribution.

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