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During early phases of a protoplanetary disks's life, gravitationalinstabilities can produce significant mass transport, can dramatically alterdisk structure, can mix and shock-process gas and solids, and may beinstrumental in planet formation. We present a 3D grid-based radiativehydrodynamics study with varied resolutions of a 0.07 M$_\odot$ disk orbiting a0.5 M$_\odot$ star as it settles over most of its radial extent into aquasi-steady asymptotic state that maintains approximate balance betweenheating produced by GIs and radiative cooling governed by realistic dustopacities. We assess disk stability criteria, thermodynamic properties,strengths of GIs, characteristics of density waves and torques produced by GIs,radial mass transport arising from these torques, and the level to whichtransport can be represented as local or nonlocal processes. Physical andthermal processes display distinct differences between inner optically thickand outer optically thin regions of the disk. In the inner region,gravitational torques are dominated by low-order Fourier components of theazimuthal mass distribution. These torques are strongly variable on the localdynamical time and are subject to rapid flaring presumably driven by recurrentswing amplification. In the outer region, m=1 torques dominate. Ring-likestructures exhibiting strong noncircular motions, and vortices develop near theinner edge between 8 and 14 au. We find that GI-induced spiral modes erupt in achaotic manner over the whole low-Q part of the disk, with many spiral modesappearing and disappearing, producing gravitoturbulence, but dominated byfluctuating large-scale modes, very different from a simple $\alpha$-disk.

Mass and Angular Momentum Transport in a Gravitationally Unstable Protoplanetary Disk with Improved 3D Radiative Hydrodynamics