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

Result code in 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>

Result on the web

<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>

Result language

angličtina

Original language name

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

Original language description

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.

Czech name

—

Czech description

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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/GA18-06083S" target="_blank" >GA18-06083S: Evolution of solid bodies in protoplanetary disks and during collisions</a><br>

Continuities

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

Publication year

2021

Confidentiality

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

Name of the periodical

Nature Astronomy [online]

ISSN

2397-3366

e-ISSN

—

Volume of the periodical

5

Issue of the periodical within the volume

9

Country of publishing house

GB - UNITED KINGDOM

Number of pages

5

Pages from-to

898-902

UT code for WoS article

000669768700005

EID of the result in the Scopus database

2-s2.0-85109869874