Gravito-Turbulent Disks in 3D: Turbulent Velocities vs. Depth

Abstract

Characterizing turbulence in protoplanetary disks is crucial for understanding how they accrete and spawn planets. Recent measurements of spectral line broadening promise to diagnose turbulence, with different lines probing different depths. We use 3D local hydrodynamic simulations of cooling, self-gravitating disks to resolve how motions driven by "gravito-turbulence" vary with height. We find that gravito-turbulence is practically as vigorous at altitude as at depth: even though gas at altitude is much too rarefied to be itself self-gravitating, it is strongly forced by self-gravitating overdensities at the midplane. The long-range nature of gravity means that turbulent velocities are nearly uniform vertically, increasing by just a factor of 2 from midplane to surface, even as the density ranges over nearly three orders of magnitude. The insensitivity of gravito-turbulence to height contrasts with the behavior of disks afflicted by the magnetorotational instability (MRI); in the latter case, non-circular velocities increase by at least a factor of 15 from midplane to surface, with various non-ideal effects only magnifying this factor. The distinct vertical profiles of gravito-turbulence vs. MRI turbulence may be used in conjunction with measurements of non-thermal linewidths at various depths to identify the source of transport in protoplanetary disks.

Accepted to ApJ

References in corpus (7)

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• Magnetic Turbulence and Thermodynamics in the Inner Region of Protoplanetary Discs
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• Dust delivery and entrainment in photoevaporative winds
• Particle Dynamics in 3D Self-gravitating Disks II: Strong Gas Accretion and Thin Dust Disks
• An Extension of the Athena++ Framework for Fully Conservative Self-Gravitating Hydrodynamics
• Gravito-turbulence in local disk simulations with an adaptive moving mesh
• The evolution of a circumplanetary disc with a dead zone
• Gravitoturbulent dynamo in global simulations of gaseous disks