NEPTUNE'S ORBITAL MIGRATION WAS GRAINY, NOT SMOOTH

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F16%3A10331708" target="_blank" >RIV/00216208:11320/16:10331708 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.3847/0004-637X/825/2/94" target="_blank" >http://dx.doi.org/10.3847/0004-637X/825/2/94</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/0004-637X/825/2/94" target="_blank" >10.3847/0004-637X/825/2/94</a>

Jazyk výsledku

angličtina

Název v původním jazyce

NEPTUNE'S ORBITAL MIGRATION WAS GRAINY, NOT SMOOTH

Popis výsledku v původním jazyce

The Kuiper Belt is a population of icy bodies beyond the orbit of Neptune. The complex orbital structure of the Kuiper Belt, including several categories of objects inside and outside of resonances with Neptune, emerged as a result of Neptune's migration into an outer planetesimal disk. An outstanding problem with the existing migration models is that they invariably predict excessively large resonant populations, while observations show that the non-resonant orbits are in fact common (e.g., the main belt population is similar or equal to 2-4 times larger than Plutinos in the 3:2 resonance). Here we show that this problem can be resolved if it is assumed that Neptune's migration was grainy, as expected from scattering encounters of Neptune with massive planetesimals. The grainy migration acts to destabilize resonant bodies with large libration amplitudes, a fraction of which ends up on stable non-resonant orbits. Thus, the non-resonant-to-resonant ratio obtained with the grainy migration is higher, up to similar to 10 times higher for the range of parameters investigated here, than in a model with smooth migration. In addition, the grainy migration leads to a narrower distribution of the libration amplitudes in the 3:2 resonance. The best fit to observations is obtained when it is assumed that the outer planetesimal disk below 30 au contained 1000-4000 Plutos. We estimate that the combined mass of Pluto-class objects in the original disk represented 10%-40% of the estimated disk mass (M-disk similar or equal to 20 M-Earth). This constraint can be used to better understand the accretion processes in the outer solar system.

Název v anglickém jazyce

NEPTUNE'S ORBITAL MIGRATION WAS GRAINY, NOT SMOOTH

Popis výsledku anglicky

The Kuiper Belt is a population of icy bodies beyond the orbit of Neptune. The complex orbital structure of the Kuiper Belt, including several categories of objects inside and outside of resonances with Neptune, emerged as a result of Neptune's migration into an outer planetesimal disk. An outstanding problem with the existing migration models is that they invariably predict excessively large resonant populations, while observations show that the non-resonant orbits are in fact common (e.g., the main belt population is similar or equal to 2-4 times larger than Plutinos in the 3:2 resonance). Here we show that this problem can be resolved if it is assumed that Neptune's migration was grainy, as expected from scattering encounters of Neptune with massive planetesimals. The grainy migration acts to destabilize resonant bodies with large libration amplitudes, a fraction of which ends up on stable non-resonant orbits. Thus, the non-resonant-to-resonant ratio obtained with the grainy migration is higher, up to similar to 10 times higher for the range of parameters investigated here, than in a model with smooth migration. In addition, the grainy migration leads to a narrower distribution of the libration amplitudes in the 3:2 resonance. The best fit to observations is obtained when it is assumed that the outer planetesimal disk below 30 au contained 1000-4000 Plutos. We estimate that the combined mass of Pluto-class objects in the original disk represented 10%-40% of the estimated disk mass (M-disk similar or equal to 20 M-Earth). This constraint can be used to better understand the accretion processes in the outer solar system.

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

—

Projekt

<a href="/cs/project/GA13-01308S" target="_blank" >GA13-01308S: Dynamika malých těles sluneční soustavy</a><br>

Návaznosti

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

Rok uplatnění

2016

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

—

Svazek periodika

825

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

18

Strana od-do

—

Kód UT WoS článku

000381940800012

EID výsledku v databázi Scopus

2-s2.0-84978512626