Kavli Affiliate: Feng Yuan
| First 5 Authors: Can Cui, Konstantin Gerbig, Ya-Ping Li, Ziyan Xu, Rixin Li
| Summary:
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.
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