Long lived dust rings around HD169142

Abstract

Recent ALMA observations of the protoplanetary disc around HD~169142 reveal a peculiar structure made of concentric dusty rings: a main ring at $\sim$20 au, a triple system of rings at $\sim 55-75$ au in millimetric continuum emission and a perturbed gas surface density from the ${}^{12}$CO,${}^{13}$CO and C${}^{18}$O$(J=2-1)$ surface brightness profile. In this Letter, we perform three-dimensional numerical simulations and radiative transfer modeling exploring the possibility that two giant planets interacting with the disc and orbiting in resonant locking can be responsible for the origin of the observed dust inner rings structure. We find that in this configuration the dust structure is actually long lived while the gas mass of the disc is accreted onto the star and the giant planets, emptying the inner region. In addition, we also find that the innermost planet is located at the inner edge of the dust ring, and can accrete mass from the disc, generating a signature in the dust ring shape that can be observed in mm ALMA observations.

8 pages, 5 figures, accepted Apj Letters

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• Dust growth, fragmentation and self-induced dust traps in PHANTOM
• Dust Traps and the Formation of Cavities in Transition Discs: A millimetre to sub-millimetre comparison survey
• Dynamical dust traps in misaligned circumbinary discs: analytical theory and numerical simulations
• A kinematic excess in the annular gap and gas depleted cavity in the disc around HD 169142
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• External or internal companion exciting the spiral arms in CQ Tau?
• The protoplanetary disc around HD 169142: circumstellar or circumbinary?
• Kinematics signature of a giant planet in the disk of AS 209
• Mapping the 3D Kinematical Structure of the Gas Disk of HD 169142