Evolution of the eccentricity and inclination of low-mass planets subjected to thermal forces: a numerical study

Kód výsledku v 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>

Výsledek na webu

<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>

Jazyk výsledku

angličtina

Název v původním jazyce

Evolution of the eccentricity and inclination of low-mass planets subjected to thermal forces: a numerical study

Popis výsledku v původním jazyce

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.

Název v anglickém jazyce

Evolution of the eccentricity and inclination of low-mass planets subjected to thermal forces: a numerical study

Popis výsledku anglicky

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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GM21-23067M" target="_blank" >GM21-23067M: Hydrodynamické interakce planet s protoplanetárními disky a původ těsných exoplanetárních soustav</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2023

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

1365-2966

Svazek periodika

522

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

15

Strana od-do

678-692

Kód UT WoS článku

000991993800038

EID výsledku v databázi Scopus

2-s2.0-85160427669