How the planetary eccentricity influences the pebble isolation mass

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F22%3A10456637" target="_blank" >RIV/00216208:11320/22:10456637 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=0L9kCIdTRu" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=0L9kCIdTRu</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stab3753" target="_blank" >10.1093/mnras/stab3753</a>

Jazyk výsledku

angličtina

Název v původním jazyce

How the planetary eccentricity influences the pebble isolation mass

Popis výsledku v původním jazyce

We investigate the pebble isolation mass (PIM) for a planet on a fixed eccentric orbit in its protoplanetary disc by conducting a set of two-dimensional (2D) hydrodynamical simulations, including dust turbulent diffusion. A range of planet eccentricities up to e = 0.2 is adopted. Our simulations also cover a range of a-turbulent viscosities, and for each pair {alpha, e} the PIM is estimated as the minimum planet mass in our simulations such that solids with a Stokes number greater than or similar to 0.05 do not flow across the planet orbit and remain trapped around a pressure bump outside the planet gap. For alpha &lt; 10(-3), we find that eccentric planets reach a well-defined PIM, which can be smaller than for planets on circular orbits when the eccentricity remains smaller than the disc&apos;s aspect ratio. We provide a fitting formula for how the PIM depends on the planet&apos;s eccentricity. However, for alpha &gt; 10(-3), eccentric planets cannot fully stall the pebbles flow and, thus, do not reach a well-defined PIM. Our results suggest that the maximum mass reached by rocky cores should exhibit a dichotomy depending on the disc&apos;s turbulent viscosity. While being limited to O(10 M-circle plus) in low-viscosity discs, this maximum mass could reach much larger values in discs with a high turbulent viscosity in the planet vicinity. Our results further highlight that pebble filtering by growing planets might not be as effective as previously thought, especially in high-viscosity discs, with important implications to protoplanetary discs observations.

Název v anglickém jazyce

How the planetary eccentricity influences the pebble isolation mass

Popis výsledku anglicky

We investigate the pebble isolation mass (PIM) for a planet on a fixed eccentric orbit in its protoplanetary disc by conducting a set of two-dimensional (2D) hydrodynamical simulations, including dust turbulent diffusion. A range of planet eccentricities up to e = 0.2 is adopted. Our simulations also cover a range of a-turbulent viscosities, and for each pair {alpha, e} the PIM is estimated as the minimum planet mass in our simulations such that solids with a Stokes number greater than or similar to 0.05 do not flow across the planet orbit and remain trapped around a pressure bump outside the planet gap. For alpha &lt; 10(-3), we find that eccentric planets reach a well-defined PIM, which can be smaller than for planets on circular orbits when the eccentricity remains smaller than the disc&apos;s aspect ratio. We provide a fitting formula for how the PIM depends on the planet&apos;s eccentricity. However, for alpha &gt; 10(-3), eccentric planets cannot fully stall the pebbles flow and, thus, do not reach a well-defined PIM. Our results suggest that the maximum mass reached by rocky cores should exhibit a dichotomy depending on the disc&apos;s turbulent viscosity. While being limited to O(10 M-circle plus) in low-viscosity discs, this maximum mass could reach much larger values in discs with a high turbulent viscosity in the planet vicinity. Our results further highlight that pebble filtering by growing planets might not be as effective as previously thought, especially in high-viscosity discs, with important implications to protoplanetary discs observations.

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

2022

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

510

Číslo periodika v rámci svazku

3

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

9

Strana od-do

3867-3875

Kód UT WoS článku

000749577000050

EID výsledku v databázi Scopus

2-s2.0-85126825520