Pebble-driven migration of low-mass planets in the 2D regime of pebble accretion

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F24%3A10491138" target="_blank" >RIV/00216208:11320/24:10491138 - isvavai.cz</a>

Result on the web

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=b03G2g.v.1" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=b03G2g.v.1</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202450922" target="_blank" >10.1051/0004-6361/202450922</a>

Result language

angličtina

Original language name

Pebble-driven migration of low-mass planets in the 2D regime of pebble accretion

Original language description

Context. Pebbles drifting past a disk-embedded low-mass planet develop asymmetries in their distribution and exert a substantial gravitational torque on the planet, thus modifying its migration rate. Aims. Our aim is to assess how the distribution of pebbles and the resulting torque change in the presence of pebble accretion, focusing on its 2D regime. Methods. First, we performed 2D high-resolution multi-fluid simulations with FARGO3D but found that they are impractical for resolving pebble accretion due to the smoothing of the planetary gravitational potential. To remove the smoothing and directly trace pebbles accreted by the planet, we developed a new code, DENEB, which evolves an ensemble of pebbles, represented by Lagrangian superparticles, in a steady-state gaseous background. Results. For small and moderate Stokes numbers, St less than or similar to 0.1, pebble accretion creates two underdense regions with a front-rear asymmetry with respect to the planet. The underdensity trailing the planet is more extended. The resulting excess of pebble mass in front of the planet then makes the pebble torque positive and capable of outperforming the negative gas torque. Pebble accretion thus enables outward migration (previously thought to occur mainly for St greater than or similar to 0.1) in a larger portion of the parameter space. It occurs for the planet mass M-pl less than or similar to 3 M-circle plus and for all the Stokes numbers considered in our study, St is an element of [10(-2), 0.785], assuming a pebble-to-gas mass ratio of Z = 0.01. Conclusions. If some of the observed planets underwent outward pebble-driven migration during their accretion, the formation sites of their progenitor embryos could have differed greatly from the usual predictions of planet formation models. To enable an update of the respective models, we provide a scaling law for the pebble torque that can be readily incorporated in N-body simulations.

Czech name

—

Czech description

—

Type

J_imp - 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)

Project

<a href="/en/project/GA21-11058S" target="_blank" >GA21-11058S: Orbital and chemical evolution of emerging planetary systems</a><br>

Continuities

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

Publication year

2024

Confidentiality

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

Name of the periodical

Astronomy &amp; Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Volume of the periodical

690

Issue of the periodical within the volume

říjen

Country of publishing house

FR - FRANCE

Number of pages

17

Pages from-to

A41

UT code for WoS article

001321174100011

EID of the result in the Scopus database

2-s2.0-85206304754