Hiding Signatures of Gravitational Instability in Protoplanetary Discs with Planets

Abstract

We carry out three dimensional SPH simulations to show that a migrating giant planet strongly suppresses the spiral structure in self-gravitating discs. We present mock ALMA continuum observations which show that in the absence of a planet, spiral arms due to gravitational instability are easily observed. Whereas in the presence of a giant planet, the spiral structures are suppressed by the migrating planet resulting in a largely axisymmetric disc with a ring and gap structure. Our modelling of the gas kinematics shows that the planet's presence could be inferred, for example, using optically thin 13C16O. Our results show that it is not necessary to limit the gas mass of discs by assuming high dust-to-gas mass ratios in order to explain a lack of spiral features that would otherwise be expected in high mass discs.

Accepted to ApJL. 9 pages, 5 figures

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• Warping Away Gravitational Instabilities in Protoplanetary Discs
• The Effect of the Approach to Gas Disk Gravitational Instability on the Rapid Formation of Gas Giant Planets. II. Quadrupled Spatial Resolution
• Continuing to Hide Signatures of Gravitational Instability in Protoplanetary Discs with Planets
• Single Fluid vs. Multifluid: Comparison between single fluid and multifluid dust models for disc planet interactions
• Molecules with ALMA at Planet-forming Scales. XX. The Massive Disk Around GM Aurigae
• Gravitational instability in planet-forming discs