Estimating the depth of gaps opened by planets in eccentric orbit

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F23%3A10475684" target="_blank" >RIV/00216208:11320/23:10475684 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=oVd.M1pvOn" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=oVd.M1pvOn</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stac2856" target="_blank" >10.1093/mnras/stac2856</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Estimating the depth of gaps opened by planets in eccentric orbit

Popis výsledku v původním jazyce

Planets can carve gaps in the surface density of protoplanetary discs. The formation of these gaps can reduce the corotation torques acting on the planets. In addition, gaps can halt the accretion of solids on to the planets as dust and pebbles can be trapped at the edge of the gap. This accumulation of dust could explain the origin of the ring-like dust structures observed using high-resolution interferometry. In this work, we provide an empirical scaling relation for the depth of the gap cleared by a planet on an eccentric orbit as a function of the planet-to-star mass ratio q, the disc aspect ratio h, Shakura-Sunyaev viscosity parameter alpha, and planetary eccentricity e. We construct the scaling relation using a heuristic approach: we calibrate a toy model based on the impulse approximation with 2D hydrodynamical simulations. The scaling reproduces the gap depth for moderate eccentricities (e &lt;= 4h) and when the surface density contrast outside and inside the gap is &lt;= 10(2). Our framework can be used as the basis of more sophisticated models aiming to predict the radial gap profile for eccentric planets.

Název v anglickém jazyce

Estimating the depth of gaps opened by planets in eccentric orbit

Popis výsledku anglicky

Planets can carve gaps in the surface density of protoplanetary discs. The formation of these gaps can reduce the corotation torques acting on the planets. In addition, gaps can halt the accretion of solids on to the planets as dust and pebbles can be trapped at the edge of the gap. This accumulation of dust could explain the origin of the ring-like dust structures observed using high-resolution interferometry. In this work, we provide an empirical scaling relation for the depth of the gap cleared by a planet on an eccentric orbit as a function of the planet-to-star mass ratio q, the disc aspect ratio h, Shakura-Sunyaev viscosity parameter alpha, and planetary eccentricity e. We construct the scaling relation using a heuristic approach: we calibrate a toy model based on the impulse approximation with 2D hydrodynamical simulations. The scaling reproduces the gap depth for moderate eccentricities (e &lt;= 4h) and when the surface density contrast outside and inside the gap is &lt;= 10(2). Our framework can be used as the basis of more sophisticated models aiming to predict the radial gap profile for eccentric planets.

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/GA21-11058S" target="_blank" >GA21-11058S: Raný orbitální a chemický vývoj planetárních 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

518

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

17

Strana od-do

439-455

Kód UT WoS článku

000900308100032

EID výsledku v databázi Scopus

2-s2.0-85147095778