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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&apos;s force arising from thermal effects) match those predicted by linear theory within similar to 20 per cent. When the planet&apos;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&apos;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

  • Czech description

Classification

  • Type

    J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database

  • CEP classification

  • 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