THE ORBITAL DISTRIBUTION OF TRANS-NEPTUNIAN OBJECTS BEYOND 50 au

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F16%3A10331711" target="_blank" >RIV/00216208:11320/16:10331711 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.3847/2041-8205/827/2/L35" target="_blank" >http://dx.doi.org/10.3847/2041-8205/827/2/L35</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/2041-8205/827/2/L35" target="_blank" >10.3847/2041-8205/827/2/L35</a>

Jazyk výsledku

angličtina

Název v původním jazyce

THE ORBITAL DISTRIBUTION OF TRANS-NEPTUNIAN OBJECTS BEYOND 50 au

Popis výsledku v původním jazyce

The dynamical structure of the Kuiper Belt beyond 50 au is not well understood. Here we report results of a numerical model with long-range, slow, and grainy migration of Neptune. The model implies that bodies scattered outward by Neptune to semimajor axes a > 50 au often evolve into resonances which subsequently act to raise the perihelion distances of orbits to q > 40 au. The implication of the model is that the orbits with 50 < a < 100 au and q > 40 au should cluster near (but not in) the resonances with Neptune (3:1 at a = 62.6 au, 4:1 at a = 75.9 au, 5:1 at a = 88.0 au, etc.). The recent detection of several distant Kuiper Belt Objects (KBOs) near resonances is consistent with this prediction, but it is not yet clear whether the orbits are really non-resonant as our model predicts. We estimate from the model that there should presently be similar to 1600-2400 bodies at the 3:1 resonance and similar to 1000-1400 bodies at the 4:1 resonance (for q > 40 au and diameters D > 100 km). These results favorably compare with the population census of distant KBOs inferred from existing observations.

Název v anglickém jazyce

THE ORBITAL DISTRIBUTION OF TRANS-NEPTUNIAN OBJECTS BEYOND 50 au

Popis výsledku anglicky

The dynamical structure of the Kuiper Belt beyond 50 au is not well understood. Here we report results of a numerical model with long-range, slow, and grainy migration of Neptune. The model implies that bodies scattered outward by Neptune to semimajor axes a > 50 au often evolve into resonances which subsequently act to raise the perihelion distances of orbits to q > 40 au. The implication of the model is that the orbits with 50 < a < 100 au and q > 40 au should cluster near (but not in) the resonances with Neptune (3:1 at a = 62.6 au, 4:1 at a = 75.9 au, 5:1 at a = 88.0 au, etc.). The recent detection of several distant Kuiper Belt Objects (KBOs) near resonances is consistent with this prediction, but it is not yet clear whether the orbits are really non-resonant as our model predicts. We estimate from the model that there should presently be similar to 1600-2400 bodies at the 3:1 resonance and similar to 1000-1400 bodies at the 4:1 resonance (for q > 40 au and diameters D > 100 km). These results favorably compare with the population census of distant KBOs inferred from existing observations.

Druh

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

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

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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 Letters

ISSN

2041-8205

e-ISSN

—

Svazek periodika

827

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

5

Strana od-do

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Kód UT WoS článku

000383712100014

EID výsledku v databázi Scopus

2-s2.0-84984677943