The behaviors of Kelvin-Helmholtz Instability in protoplanetary disks

Details The behaviors of Kelvin-Helmholtz Instability in protoplanetary disks The behaviors of Kelvin-Helmholtz Instability in protoplanetary disks

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.7604k&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #76.04; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

We investigate the behaviors of the Kelvin-Helmholtz instability (hereafter KHI) in protolanetary discs by two dimensional simulations in a local box using CIP method. The excitation of KHI is expected at the inner-edge of the disk (Nakamura et al., this meeting). We find that the KH turbulence in a rotating frame develops differently from those of ordinary cases in a non-rotating frame. The gas in the rotating disc is under the balance between central gravity, centrifugal force and the pressure gradient. When a vortex is induced by the KHI, the modification to this pre-existing structure, which does not exist in an ordinary situation, leads to gas mixing over a much longer distance in the radial direction. This is due to the following two effects, (1) the Coriolis force acts as a buoyancy force so that a low density part of the vortex drifts radially outward. (2) Coriolis force is reduced such that it cannot balance against the gravity, making a dense part of the vortex to fall inward. These effects become stronger when the density contrast across the shear layer is large. Indeed a large density jump is expected at the disk-inner edge. The growth time scale of KHI is as fast as the orbital time implying that the local velocity shear layer dynamics at the inner-edge would develop quickly to have large-scale impacts over a substantial part of the disk.

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