Low-mass planets falling into gaps with cyclonic vortices
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F24%3A10492995" target="_blank" >RIV/00216208:11320/24:10492995 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=XXDkaoBK59" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=XXDkaoBK59</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/stae1548" target="_blank" >10.1093/mnras/stae1548</a>
Alternative languages
Result language
angličtina
Original language name
Low-mass planets falling into gaps with cyclonic vortices
Original language description
We investigate the planetary migration of low-mass planets ($M_pin [1,15], mathrm{ M}_{oplus }$, here $mathrm{ M}_{oplus }$ is the Earth mass) in a gaseous disc containing a previously formed gap. We perform high-resolution 3D simulations with the fargo3d code. To create the gap in the surface density of the disc, we use a radial viscosity profile with a bump, which is maintained during the entire simulation time. We find that when the gap is sufficiently deep, the spiral waves excited by the planet trigger the Rossby wave instability, forming cyclonic (underdense) vortices at the edges of the gap. When the planet approaches the gap, it interacts with the vortices, which produce a complex flow structure around the planet. Remarkably, we find a widening of the horseshoe region of the planet produced by the vortex at the outer edge of the gap, which depending on the mass of the planet differs by at least a factor of two with respect to the standard horseshoe width. This inevitably leads to an increase in the co-rotation torque on the planet and produces an efficient trap to halt its inward migration. In some cases, the planet becomes locked in co-rotation with the outer vortex. Under this scenario, our results could explain why low-mass planets do not fall towards the central star within the lifetime of the protoplanetary disc. Lastly, the development of these vortices produces an asymmetric temporal evolution of the gap, which could explain the structures observed in some protoplanetary discs.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/GM21-23067M" target="_blank" >GM21-23067M: Hydrodynamic interactions of planets with protoplanetary disks and the origin of close-in exoplanetary systems</a><br>
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Others
Publication year
2024
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Monthly Notices of the Royal Astronomical Society
ISSN
0035-8711
e-ISSN
1365-2966
Volume of the periodical
532
Issue of the periodical within the volume
2
Country of publishing house
GB - UNITED KINGDOM
Number of pages
16
Pages from-to
1345-1360
UT code for WoS article
001265147500001
EID of the result in the Scopus database
2-s2.0-85198253437