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Published February 1, 2016 | Published + Submitted
Journal Article Open

On Shocks Driven by High-mass Planets in Radiatively Inefficient Disks. II. Three-dimensional Global Disk Simulations

Abstract

Recent high-resolution, near-infrared images of protoplanetary disks have shown that these disks often present spiral features. Spiral arms are among the structures predicted by models of disk–planet interaction and thus it is tempting to suspect that planetary perturbers are responsible for these signatures. However, such interpretation is not free of problems. The observed spirals have large pitch angles, and in at least one case (HD 100546) it appears effectively unpolarized, implying thermal emission of the order of 1000 K (465 ± 40 K at closer inspection). We have recently shown in two-dimensional models that shock dissipation in the supersonic wake of high-mass planets can lead to significant heating if the disk is sufficiently adiabatic. Here we extend this analysis to three dimensions in thermodynamically evolving disks. We use the Pencil Code in spherical coordinates for our models, with a prescription for thermal cooling based on the optical depth of the local vertical gas column. We use a 5M_J planet, and show that shocks in the region around the planet where the Lindblad resonances occur heat the gas to substantially higher temperatures than the ambient gas. The gas is accelerated vertically away from the midplane to form shock bores, and the gas falling back toward the midplane breaks up into a turbulent surf. This turbulence, although localized, has high α values, reaching 0.05 in the inner Lindblad resonance, and 0.1 in the outer one. We find evidence that the disk regions heated up by the shocks become superadiabatic, generating convection far from the planet's orbit.

Additional Information

© 2016 The American Astronomical Society. Received 2015 September 24; accepted 2015 November 12; published 2016 January 26. The simulations presented here were carried out using the Stampede cluster of the Texas Advanced Computing Center (TACC) at The University of Texas at Austin through XSEDE grant TG-AST140014. M-MML was partly supported by NASA grant NNX14AJ56G and the Humboldt Foundation. We acknowledge discussions with Thayne Currie and thank the anonymous referee for helpful comments. This work was performed in part at the Jet Propulsion Laboratory, California Institute of Technology. N.J.T. was supported by grant 13-OSS13-0114 from the NASA Origins of the Solar System program.

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Published - Lyra_2016p102.pdf

Submitted - 1511.02988v2.pdf

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