Early terrestrial planet formation by torque-driven convergent migration of planetary embryos

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F21%3A10438658" target="_blank" >RIV/00216208:11320/21:10438658 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=uwsoHlcL63" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=uwsoHlcL63</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1038/s41550-021-01383-3" target="_blank" >10.1038/s41550-021-01383-3</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Early terrestrial planet formation by torque-driven convergent migration of planetary embryos

Popis výsledku v původním jazyce

The massive cores of the giant planets are thought to have formed in a gas disk by the accretion of pebble-sized particles whose accretional cross-section was enhanced by aerodynamic gas drag(1,2). A commonly held view is that the terrestrial planet system formed later (30-200 Myr after the dispersal of the gas disk) by giant collisions of tens of lunar-to Mars-sized protoplanets(3,4). Here we propose, instead, that the terrestrial planets of the Solar System formed earlier by the gas-driven convergent migration of protoplanets towards similar to 1 au. To investigate situations in which convergent migration occurs and determine the thermal structure of the gas and pebble disks in the terrestrial planet zone, we developed a radiation-hydrodynamic model with realistic opacities(5,6). We find that protoplanets grow in the first 10 Myr by mutual collisions and pebble accretion, and gain orbital eccentricities by gravitational scattering and the hot-trail effect(7,8). The orbital structure of the inner Solar System is well reproduced in our simulations, including its tight mass concentration at 0.7-1 au and the small sizes of Mercury and Mars. The early-stage protosolar disk temperature exceeds 1,500 K inside 0.4 au, implying that Mercury grew in a highly reducing environment next to the evaporation lines of iron and silicates, influencing Mercury&apos;s bulk composition(9). A dissipating gas disk, however, is cold, and pebbles drifting from larger heliocentric distances would deliver volatile elements.

Název v anglickém jazyce

Early terrestrial planet formation by torque-driven convergent migration of planetary embryos

Popis výsledku anglicky

The massive cores of the giant planets are thought to have formed in a gas disk by the accretion of pebble-sized particles whose accretional cross-section was enhanced by aerodynamic gas drag(1,2). A commonly held view is that the terrestrial planet system formed later (30-200 Myr after the dispersal of the gas disk) by giant collisions of tens of lunar-to Mars-sized protoplanets(3,4). Here we propose, instead, that the terrestrial planets of the Solar System formed earlier by the gas-driven convergent migration of protoplanets towards similar to 1 au. To investigate situations in which convergent migration occurs and determine the thermal structure of the gas and pebble disks in the terrestrial planet zone, we developed a radiation-hydrodynamic model with realistic opacities(5,6). We find that protoplanets grow in the first 10 Myr by mutual collisions and pebble accretion, and gain orbital eccentricities by gravitational scattering and the hot-trail effect(7,8). The orbital structure of the inner Solar System is well reproduced in our simulations, including its tight mass concentration at 0.7-1 au and the small sizes of Mercury and Mars. The early-stage protosolar disk temperature exceeds 1,500 K inside 0.4 au, implying that Mercury grew in a highly reducing environment next to the evaporation lines of iron and silicates, influencing Mercury&apos;s bulk composition(9). A dissipating gas disk, however, is cold, and pebbles drifting from larger heliocentric distances would deliver volatile elements.

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/GA18-06083S" target="_blank" >GA18-06083S: Vývoj pevných těles v protoplanetárních discích a během kolizí</a><br>

Návaznosti

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

Rok uplatnění

2021

Kód důvěrnosti údajů

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

Název periodika

Nature Astronomy [online]

ISSN

2397-3366

e-ISSN

—

Svazek periodika

5

Číslo periodika v rámci svazku

9

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

5

Strana od-do

898-902

Kód UT WoS článku

000669768700005

EID výsledku v databázi Scopus

2-s2.0-85109869874