Evolution of the eccentricity and inclination of low-mass planets subjected to thermal forces: a numerical study
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F23%3A10475690" target="_blank" >RIV/00216208:11320/23:10475690 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=UgkF1notpY" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=UgkF1notpY</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/stad681" target="_blank" >10.1093/mnras/stad681</a>
Alternative languages
Result language
angličtina
Original language name
Evolution of the eccentricity and inclination of low-mass planets subjected to thermal forces: a numerical study
Original language description
By means of three-dimensional high-resolution hydrodynamical simulations, we study the orbital evolution of weakly eccentric or inclined low-mass protoplanets embedded in gaseous discs subject to thermal diffusion. We consider both non-luminous planets and planets that also experience the radiative feedback from their own luminosity. We compare our results to previous analytical work and find that thermal forces (the contribution to the disc's force arising from thermal effects) match those predicted by linear theory within similar to 20 per cent. When the planet's luminosity exceeds a threshold found to be within 10 per cent of that predicted by linear theory, its eccentricity and inclination grow exponentially, whereas these quantities undergo a strong damping below this threshold. In this regime of low luminosity indeed, thermal diffusion cools the surroundings of the planet and allows gas to accumulate in its vicinity. It is the dynamics of this gas excess that contributes to damp eccentricity and inclination. The damping rates obtained can be up to h(-1) times larger than those due to the resonant interaction with the disc, where h is the disc's aspect ratio. This suggests that models that incorporate planet-disc interactions using well-known formulae based on resonant wave-launching to describe the evolution of eccentricity and inclination underestimate the damping action of the disc on the eccentricity and inclination of low-mass planets by an order of magnitude.
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
2023
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
522
Issue of the periodical within the volume
1
Country of publishing house
GB - UNITED KINGDOM
Number of pages
15
Pages from-to
678-692
UT code for WoS article
000991993800038
EID of the result in the Scopus database
2-s2.0-85160427669