Dust Growth in ALMA Rings: II. Dusty Rossby Wave Instability

Abstract

Annular substructures serve as ideal venues for planetesimal formation. In this series, we investigate the linear stage of dust growth within rings. The first paper examines the global streaming instability, while this study focuses on the dusty Rossby wave instability (DRWI). We perform a linear analysis of the two-fluid equations on a background pressure bump, representing annular substructures. The spectral code \textsc{Dedalus} is used to solve the linear eigenvalue problem. We identify two distinct DRWI modes: Type I, which originates from dust-modified gas RWI, and Type II, which results from dust-gas coupling. These modes never coexist for a given azimuthal wavenumber $\ky$, but transition between each other as $\ky$ varies. Type I modes are driven by the advection of background vorticity, whereas Type II modes involve two primary waves: Rossby waves, driven by advection, and thin waves, driven by dust-gas drag. Finally, we assess the relevance of DRWI in ALMA rings using DSHARP sources. Our findings suggest that Type I modes could explain the absence of azimuthal asymmetries in many ALMA disks, whereas Type II modes are entirely absent in all eight observed rings, implying that unresolved narrow rings or alternative mechanisms may play a role in dust growth within annular substructures.

24 pages, 15 figures, accepted to ApJ, DOI: 10.3847/1538-4357/add146

References in corpus (33)

• Gas- and dust evolution in protoplanetary disks
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• Two accreting protoplanets around the young star PDS 70
• The stickiness of micrometer-sized water-ice particles
• A Three-Dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk using DCO${}^{+}$
• How to form planetesimals from mm-sized chondrules and chondrule aggregates
• Initial mass function of planetesimals formed by the streaming instability
• Measuring turbulent motion in planet-forming disks with ALMA: A detection around DM Tau and non-detections around MWC 480 and V4046 Sgr
• 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
• Dust growth and evolution in protoplanetary disks
• Turbulence sets the length scale for planetesimal formation: Local 2D simulations of streaming instability and planetesimal formation
• Empirical constraints on turbulence in proto-planetary discs
• Including Dust Coagulation in Hydrodynamic Models of Protoplanetary Disks: Dust Evolution in the Vicinity of a Jupiter-mass Planet
• The efficiency of dust trapping in ringed proto-planetary discs
• Frankenstein: Protoplanetary disc brightness profile reconstruction at sub-beam resolution with a rapid Gaussian process
• A thermodynamic view of dusty protoplanetary disks
• Global Three-Dimensional Simulations of Outer Protoplanetary Disks with Ambipolar Diffusion
• Spontaneous ring formation in wind-emitting accretion discs
• Slowly-growing gap-opening planets trigger weaker vortices
• Local models of astrophysical discs
• A super-resolution analysis of the DSHARP survey: Substructure is common in the inner 30 au
• Dust Settling and Clumping in MRI Turbulent Outer Protoplanetary Disks
• Turbulence in outer protoplanetary disks: MRI or VSI?
• Formation of Dust Rings and Gaps in Non-ideal MHD Disks Through Meridional Gas Flows
• Planetesimal Initial Mass Functions following Diffusion Regulated Gravitational Collapse
• Turbulent Dust-trapping Rings as Efficient Sites for Planetesimal Formation
• On the Vertical Shear Instability in Magnetized Protoplanetary Disks
• Emergence of vortices at the edges of planet-driven gaps in protoplanetary discs
• On Secular Gravitational Instability in Vertically Stratified Disks
• Stability of Dusty Rings in Protoplanetary Discs
• Rossby wave instability in weakly ionized protoplanetary disks. II. radial B-fields
• Developing a Non-Newtonian Fluid Model for Dust, for Application to Astrophysical Flows