Gravito-turbulence in irradiated protoplanetary discs

Abstract

Using radiation hydrodynamics simulations in a local stratified shearing box with realistic equations of state and opacities, we explored the outcome of self-gravity at 50 AU in a protoplanetary disc irradiated by the central star. We found that gravito-turbulence is sustained for a finite range of the surface density, from $\sim 80$ to $\sim$ 250 gcm${}^{-2}$. The disk is laminar below the range while fragments above it. In the range of gravito-turbulence, the Toomre parameter decreases monotonically from $\sim 1$ to $\sim 0.7$ as the surface density increases while an effective cooling time is almost constant at $\sim 4$ in terms of the inverse of the orbital frequency. The turbulent motions are supersonic at all heights, which dissipates through both shock waves and compressional heating. The compressional motions, occurring near the midplane, create upward flows, which not only contribute to supporting the disc but also to transporting the dissipated energy to the disc surfaces. The irradiation does not affect much the gravito-turbulence near the midplane unless the grazing angle is larger than 0.32. We also show that a simple cooling function with a constant cooling time does not approximate the realistic cooling.

accepted for publication in MNRAS

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• Gravito-turbulence and the excitation of small-scale parametric instability in astrophysical discs
• Gravitoturbulent dynamos in astrophysical discs
• Nonlinear outcome of gravitational instability in an irradiated protoplanetary disc
• Spiral structures in gravito-turbulent gaseous disks
• Investigating Protoplanetary Disk Cooling through Kinematics: Analytical GI Wiggle
• Particle Dynamics in 3D Self-gravitating Disks I: Spirals
• Vertical shear instability with dust evolution and consistent cooling times. On the importance of the initial dust distribution