On the Azimuthal Structure of Thermal Convection in Circumstellar Disks

Details On the Azimuthal Structure of Thermal Convection in Circumstellar Disks On the Azimuthal Structure of Thermal Convection in Circumstellar Disks

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...514..325k&link_type=abstract

The Astrophysical Journal, Volume 514, Issue 1, pp. 325-343.

Astronomy and Astrophysics

Astronomy

35

Accretion, Accretion Disks, Stars: Circumstellar Matter, Convection, Hydrodynamics, Methods: Numerical

Scientific paper

We study the three-dimensional (3D) global structure of thermal convection in a protoplanetary accretion disk. For that purpose, we have developed a new, versatile 3D hydrocode that incorporates radiation transport and tensor viscosity in different coordinate systems. The code was extensively tested internally by recalculating the most recent models of circumstellar disk convection. With our new code we were able, for the first time, to simulate the large-scale (azimuthal) structure of circumstellar disk convection as it will develop under the assumption of an alpha viscosity. We find that axisymmetry is broken and convective motions with an azimuthal wavelength of about 4 pressure scale heights form.

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