Modeling the arc and ring structures in the HD 143006 disk

Abstract

Rings and asymmetries in protoplanetary disks are considered as signposts of ongoing planet formation. In this work, we conduct three-dimensional radiative transfer simulations to model the intriguing disk around HD 143006 that has three dust rings and a bright arc. A complex geometric configuration, with a misaligned inner disk, is assumed to account for the asymmetric structures. The two-dimensional surface density is constructed by iteratively fitting the ALMA data. We find that the dust temperature displays a notable discontinuity at the boundary of the misalignment. The ring masses range from 0.6 to 16Mearth that are systematically lower than those inferred in the younger HL Tau disk. The arc occupies nearly 20% of the total dust mass. Such a high mass fraction of dust grains concentrated in a local region is consistent with the mechanism of dust trapping into vortices. Assuming a gas-to-dust mass ratio of 30 that is constant throughout the disk, the dense and cold arc is close to the threshold of being gravitationally unstable, with the Toomre parameter Q~1.3. Nevertheless, our estimate of Q relies on the assumption for the unknown gas-to-dust mass ratio. Adopting a lower gas-to-dust mass ratio would increase the inferred Q value. Follow-up high resolution observations of dust and gas lines are needed to clarify the origin of the substructures.

12 Pages, 8 figures, Accepted for publication in Science China Physics, Mechanics & Astronomy

References in corpus (24)

• The Transiting Exoplanet Survey Satellite
• Spiral Density Waves in a Young Protoplanetary Disk
• Evidence of fast pebble growth near condensation fronts in the HL Tau protoplanetary disk
• A Submillimeter View of Circumstellar Dust Disks in $\rho$ Ophiuchus
• Asymmetric features in the protoplanetary disk MWC758
• A Three-Dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk using DCO${}^{+}$
• Close-in planetesimal formation by pile-up of drifting pebbles
• Three radial gaps in the disk of TW Hydrae imaged with SPHERE
• Shadows and spirals in the protoplanetary disk HD 100453
• One Solution to the Mass Budget Problem for Planet Formation: Optically Thick Disks with Dust Scattering
• Results of the ROTOR-program. I. The long-term photometric variability of classical T Tauri stars
• The Disk Substructures at High Angular Resolution Project (DSHARP): III. Spiral Structures in the Millimeter Continuum of the Elias 27, IM Lup, and WaOph 6 Disks
• The newborn planet population emerging from ring-like structures in discs
• Magnetic Flux Concentration and Zonal Flows in Magnetorotational Instability Turbulence
• Dust Trapping by Vortices in Transitional Disks: Evidence for Non-ideal MHD Effects in Protoplanetary Disks
• Thermal desorption of circumstellar and cometary ice analogs
• Signatures of broken protoplanetary discs in scattered light and in sub-millimetre observations
• No Clear, Direct Evidence for Multiple Protoplanets Orbiting LkCa 15: LkCa 15 bcd are Likely Inner Disk Signals
• The Formation and Evolution of Planetary Systems: Description of the Spitzer Legacy Science Database
• Global Three-Dimensional Simulations of Outer Protoplanetary Disks with Ambipolar Diffusion
• Long Term Evolution of Planet-Induced Vortices in Protoplanetary Disks
• The properties of the inner disk around HL Tau: Multi-wavelength modeling of the dust emission
• HD 143006: circumbinary planet or misaligned disc?
• Dust concentration and emission in protoplanetary disks vortices

Cited by in corpus (2)

• Millimeter Gap Contrast as a Probe for Turbulence Level in Protoplanetary Disks
• Discovery of Two Different Full Disk Evolutionary Patterns of M-type T Tauri Stars with LAMOST DR8