Filament Formation due to Diffusive Instabilities in Dusty Protoplanetary Disks
We report the finding of a new, local diffusion instability in a protoplanetary disk which can operate in a dust fluid, subject to mass diffusion, shear viscosity, and dust–gas drag, provided the diffusivity, viscosity, or both, decrease sufficiently rapidly with increasing dust surface mass density...
| Main Authors: | , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad1114 |
| _version_ | 1797346836889993216 |
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| author | Konstantin Gerbig Min-Kai Lin Marius Lehmann |
| author_facet | Konstantin Gerbig Min-Kai Lin Marius Lehmann |
| author_sort | Konstantin Gerbig |
| collection | DOAJ |
| description | We report the finding of a new, local diffusion instability in a protoplanetary disk which can operate in a dust fluid, subject to mass diffusion, shear viscosity, and dust–gas drag, provided the diffusivity, viscosity, or both, decrease sufficiently rapidly with increasing dust surface mass density. We devise a vertically averaged, axisymmetric hydrodynamic model to describe a dense, midplane dust layer in a protoplanetary disk. The gas is modeled as a passive component, imposing an effective, diffusion-dependent pressure, mass diffusivity, and viscosity onto the otherwise collisionless dust fluid, via turbulence excited by the gas alone, or dust and gas in combination. In particular, we argue that such conditions are met when the dust–gas mixture generates small-scale turbulence through the streaming instability, as supported by recent measurements of dust mass diffusion slopes in simulations. We hypothesize that the newly discovered instability may be the origin of filamentary features, almost ubiquitously found in simulations of the streaming instability. In addition, our model allows for growing oscillatory modes, which operate in a similar fashion as the axisymmetric viscous overstability in dense planetary rings. However, it remains speculative if the required conditions for such modes can be met in protoplanetary disks. |
| first_indexed | 2024-03-08T11:38:56Z |
| format | Article |
| id | doaj.art-e77a41162acb44638856ab63ff5b470d |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-08T11:38:56Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-e77a41162acb44638856ab63ff5b470d2024-01-25T11:21:30ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01961218310.3847/1538-4357/ad1114Filament Formation due to Diffusive Instabilities in Dusty Protoplanetary DisksKonstantin Gerbig0https://orcid.org/0000-0002-4836-1310Min-Kai Lin1https://orcid.org/0000-0002-8597-4386Marius Lehmann2https://orcid.org/0000-0002-0496-3539Department of Astronomy, Yale University , New Haven, CT 06511, USA ; konstantin.gerbig@yale.eduInstitute of Astronomy and Astrophysics , Academia Sinica, Taipei 10617, Taiwan; Physics Division, National Center for Theoretical Sciences , Taipei 10617, TaiwanInstitute of Astronomy and Astrophysics , Academia Sinica, Taipei 10617, TaiwanWe report the finding of a new, local diffusion instability in a protoplanetary disk which can operate in a dust fluid, subject to mass diffusion, shear viscosity, and dust–gas drag, provided the diffusivity, viscosity, or both, decrease sufficiently rapidly with increasing dust surface mass density. We devise a vertically averaged, axisymmetric hydrodynamic model to describe a dense, midplane dust layer in a protoplanetary disk. The gas is modeled as a passive component, imposing an effective, diffusion-dependent pressure, mass diffusivity, and viscosity onto the otherwise collisionless dust fluid, via turbulence excited by the gas alone, or dust and gas in combination. In particular, we argue that such conditions are met when the dust–gas mixture generates small-scale turbulence through the streaming instability, as supported by recent measurements of dust mass diffusion slopes in simulations. We hypothesize that the newly discovered instability may be the origin of filamentary features, almost ubiquitously found in simulations of the streaming instability. In addition, our model allows for growing oscillatory modes, which operate in a similar fashion as the axisymmetric viscous overstability in dense planetary rings. However, it remains speculative if the required conditions for such modes can be met in protoplanetary disks.https://doi.org/10.3847/1538-4357/ad1114Protoplanetary disksPlanet formationCircumstellar dustHydrodynamicsAstrophysical dust processesAstrophysical fluid dynamics |
| spellingShingle | Konstantin Gerbig Min-Kai Lin Marius Lehmann Filament Formation due to Diffusive Instabilities in Dusty Protoplanetary Disks The Astrophysical Journal Protoplanetary disks Planet formation Circumstellar dust Hydrodynamics Astrophysical dust processes Astrophysical fluid dynamics |
| title | Filament Formation due to Diffusive Instabilities in Dusty Protoplanetary Disks |
| title_full | Filament Formation due to Diffusive Instabilities in Dusty Protoplanetary Disks |
| title_fullStr | Filament Formation due to Diffusive Instabilities in Dusty Protoplanetary Disks |
| title_full_unstemmed | Filament Formation due to Diffusive Instabilities in Dusty Protoplanetary Disks |
| title_short | Filament Formation due to Diffusive Instabilities in Dusty Protoplanetary Disks |
| title_sort | filament formation due to diffusive instabilities in dusty protoplanetary disks |
| topic | Protoplanetary disks Planet formation Circumstellar dust Hydrodynamics Astrophysical dust processes Astrophysical fluid dynamics |
| url | https://doi.org/10.3847/1538-4357/ad1114 |
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