Modeling the nonaxisymmetric structure in the HD 163296 disk with planet-disk interaction

TL;DR

This study uses hydrodynamical simulations and radiative transfer modeling to explore how planet-disk interactions can produce crescent-shaped asymmetries in the HD 163296 protoplanetary disk, providing insights into planet formation.

Contribution

It demonstrates that a Jupiter-mass planet can create observed asymmetries, constrains planet properties, and highlights the role of disk viscosity and dust feedback in such features.

Findings

A Jupiter-mass planet at 48 au can produce the crescent asymmetry.

Low disk viscosity ($ imes 10^{-3}$) is necessary for feature stability.

Dust feedback has a negligible effect on the observed asymmetry.

Abstract

High resolution ALMA observations revealed a variety of rich substructures in numerous protoplanetary disks. These structures consist of rings, gaps and asymmetric features. It is debated whether planets can be accounted for these substructures in the dust continuum. Characterizing the origin of asymmetries as seen in HD 163296 might lead to a better understanding of planet formation and the underlying physical parameters of the system. We test the possibility of the formation of the crescent-shaped asymmetry in the HD 163296 disk through planet-disk interaction. The goal is to obtain constraints on planet masses and eccentricities and disk viscosities. Two dimensional, multi-fluid, hydrodynamical simulations are performed with the FARGO3D code including three embedded planets. Dust is described with the pressureless fluid approach and is distributed over eight size bins. Resulting grids are post-processed with the radiative transfer code RADMC-3D and the CASA software to model synthetic observations. We find that the crescent-shaped asymmetry can be qualitatively modeled with a Jupiter mass planet at a radial distance of 48 au. Dust is trapped preferably in the trailing Lagrange point L5 with a mass of 10 to 15 earth masses. Increased values of eccentricity of the innermost Jupiter mass planet damages the stability of the crescent-shaped feature and does not reproduce the observed radial proximity to the first prominent ring in the system. Generally, a low level of viscosity ($\alpha \leq 2\cdot10^{-3}$) is necessary to allow the existence of such a feature. Including dust feedback the leading point L4 can dominantly capture dust for dust grains with an initial Stokes number $\leq 3.6\cdot 10^{-2}$. The observational results suggest a negligible effect of dust feedback since only one such feature has been detected so far.