“Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability
The Rossby wave instability (RWI) is the fundamental nonaxisymmetric radial shear instability in disks. The RWI can facilitate disk accretion, set the shape of planetary gaps, and produce large vortices. It arises from density and/or temperature features, such as radial gaps, bumps, or steps. A gene...
Saved in:
| Main Authors: | , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2024-01-01
|
| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/ad81f6 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1846167986392530944 |
|---|---|
| author | Eonho Chang Andrew N. Youdin |
| author_facet | Eonho Chang Andrew N. Youdin |
| author_sort | Eonho Chang |
| collection | DOAJ |
| description | The Rossby wave instability (RWI) is the fundamental nonaxisymmetric radial shear instability in disks. The RWI can facilitate disk accretion, set the shape of planetary gaps, and produce large vortices. It arises from density and/or temperature features, such as radial gaps, bumps, or steps. A general, sufficient condition to trigger the RWI is lacking, which we address by studying the linear RWI in a suite of simplified models, including incompressible and compressible shearing sheets and global, cylindrical disks. We focus on enthalpy amplitude and width as the fundamental properties of disk features with various shapes. We find analytic results for the RWI boundary and growth rates across a wide parameter space, in some cases with exact derivations and in others as a description of numerical results. Features wider than a scale height generally become unstable about halfway to Rayleigh instability, i.e., when the squared epicyclic frequency is about half the Keplerian value, reinforcing our previous finding. RWI growth rates approximately scale as enthalpy amplitude to the 1/3 power, with a weak dependence on width, across much of the parameter space. Global disk curvature affects wide planetary gaps, making the outer gap edge more susceptible to the RWI. Our simplified models are barotropic and height integrated, but the main results should carry over to more complex and realistic scenarios. |
| format | Article |
| id | doaj-art-a35b5f700d864e6695eb1fe8bc2bb3d4 |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-a35b5f700d864e6695eb1fe8bc2bb3d42024-11-14T12:03:21ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01976110010.3847/1538-4357/ad81f6“Halfway to Rayleigh” and Other Insights into the Rossby Wave InstabilityEonho Chang0https://orcid.org/0000-0003-4703-2053Andrew N. Youdin1https://orcid.org/0000-0002-3644-8726Graduate Interdisciplinary Program in Applied Mathematics, University of Arizona , Tucson, AZ 85721, USA; Department of Astronomy and Steward Observatory, University of Arizona , Tucson, AZ 85721, USADepartment of Astronomy and Steward Observatory, University of Arizona , Tucson, AZ 85721, USA; Lunar and Planetary Laboratory, University of Arizona , Tucson, AZ 85721, USAThe Rossby wave instability (RWI) is the fundamental nonaxisymmetric radial shear instability in disks. The RWI can facilitate disk accretion, set the shape of planetary gaps, and produce large vortices. It arises from density and/or temperature features, such as radial gaps, bumps, or steps. A general, sufficient condition to trigger the RWI is lacking, which we address by studying the linear RWI in a suite of simplified models, including incompressible and compressible shearing sheets and global, cylindrical disks. We focus on enthalpy amplitude and width as the fundamental properties of disk features with various shapes. We find analytic results for the RWI boundary and growth rates across a wide parameter space, in some cases with exact derivations and in others as a description of numerical results. Features wider than a scale height generally become unstable about halfway to Rayleigh instability, i.e., when the squared epicyclic frequency is about half the Keplerian value, reinforcing our previous finding. RWI growth rates approximately scale as enthalpy amplitude to the 1/3 power, with a weak dependence on width, across much of the parameter space. Global disk curvature affects wide planetary gaps, making the outer gap edge more susceptible to the RWI. Our simplified models are barotropic and height integrated, but the main results should carry over to more complex and realistic scenarios.https://doi.org/10.3847/1538-4357/ad81f6HydrodynamicsAstrophysical fluid dynamicsPlanet formationProtoplanetary disks |
| spellingShingle | Eonho Chang Andrew N. Youdin “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability The Astrophysical Journal Hydrodynamics Astrophysical fluid dynamics Planet formation Protoplanetary disks |
| title | “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability |
| title_full | “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability |
| title_fullStr | “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability |
| title_full_unstemmed | “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability |
| title_short | “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability |
| title_sort | halfway to rayleigh and other insights into the rossby wave instability |
| topic | Hydrodynamics Astrophysical fluid dynamics Planet formation Protoplanetary disks |
| url | https://doi.org/10.3847/1538-4357/ad81f6 |
| work_keys_str_mv | AT eonhochang halfwaytorayleighandotherinsightsintotherossbywaveinstability AT andrewnyoudin halfwaytorayleighandotherinsightsintotherossbywaveinstability |