Disk‐Planet Interaction Simulations. I. Baroclinic Generation of Vortensity and Nonaxisymmetric Rossby Wave Instability
| Autor: | Lin Liu, Xiaomeng Peng, Shangli Ou, Jianghui Ji |
|---|---|
| Rok vydání: | 2007 |
| Předmět: |
Physics
010504 meteorology & atmospheric sciences Baroclinity Astrophysics (astro-ph) Rossby wave Giant planet FOS: Physical sciences Astronomy and Astrophysics Astrophysics Protoplanetary disk 01 natural sciences Instability Physics::Fluid Dynamics 13. Climate action Space and Planetary Science Planet Potential vorticity Barotropic fluid 0103 physical sciences Astrophysics::Earth and Planetary Astrophysics 010303 astronomy & astrophysics 0105 earth and related environmental sciences |
| Zdroj: | The Astrophysical Journal. 667:1220-1228 |
| ISSN: | 1538-4357 0004-637X |
| Popis: | We use a multi-dimensional hydrodynamics code to study the gravitational interaction between an embedded planet and a protoplanetary disk with emphasis on the generation of vortensity (potential vorticity) through a Baroclinic Instability and subsequent development of Rossby-Wave-Instability (RWI). It is found that the generation of potential vorticity is very common and effective in non-barotropic disks through the Baroclinic Instability, especially within the coorbital region. Our results also complement previous studies by \citet{KLL03} that non-axisymmetric RWIs are likely to develop at local minima of potential vorticity distribution that are generated by the interaction between a planet and a inviscid barotropic disk. This second instability appears to be very common and robust, regardless of the equation of state, initial density distribution, and rotational law of the disk. The development of RWIs results in non-axisymmetric density blobs, which exert stronger torques onto the planet when they travel in the vicinity of the planet. As a result of that, large amplitude oscillations are introduced to the time behavior of the total torque acted on the planet by the disk. In our current simulations, RWIs do not change the overall picture of inward orbital migration but bring in a non-monotonic behavior to the migration speed. As a side effect, RWIs also introduce interesting structures into the disk. These structures may help the formation of Earth-like planets in the Habitable Zone or Hot Earths interior to a close-in giant planet. ~ 30 pages, Ap. J. in press |
| Databáze: | OpenAIRE |
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