TILTING JUPITER (A BIT) AND SATURN (A LOT) DURING PLANETARY MIGRATION

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F15%3A10314994" target="_blank" >RIV/00216208:11320/15:10314994 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1088/0004-637X/806/1/143" target="_blank" >http://dx.doi.org/10.1088/0004-637X/806/1/143</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1088/0004-637X/806/1/143" target="_blank" >10.1088/0004-637X/806/1/143</a>

Jazyk výsledku

angličtina

Název v původním jazyce

TILTING JUPITER (A BIT) AND SATURN (A LOT) DURING PLANETARY MIGRATION

Popis výsledku v původním jazyce

We study the effects of planetary late migration on the gas giants' obliquities. We consider the planetary instability models from Nesvorny and Morbidelli, in which the obliquities of Jupiter and Saturn can be excited when spin-orbit resonances occur. The most notable resonances occur when the s(7) and s(8) frequencies, changing as a result of planetary migration, become commensurate with the precession frequencies of Jupiter's and Saturn's spin vectors. We show that Jupiter may have obtained its present obliquity by crossing of the s(8) resonance. This would set strict constraints on the character of migration during the early stage. Additional effects on Jupiter's obliquity are expected during the last gasp of migration when the s(7) resonance was approached. The magnitude of these effects depends on the precise value of the Jupiter's precession constant. Saturn's large obliquity was likely excited by capture into the s(8) resonance. This probably happened during the late stage of pl

Název v anglickém jazyce

TILTING JUPITER (A BIT) AND SATURN (A LOT) DURING PLANETARY MIGRATION

Popis výsledku anglicky

We study the effects of planetary late migration on the gas giants' obliquities. We consider the planetary instability models from Nesvorny and Morbidelli, in which the obliquities of Jupiter and Saturn can be excited when spin-orbit resonances occur. The most notable resonances occur when the s(7) and s(8) frequencies, changing as a result of planetary migration, become commensurate with the precession frequencies of Jupiter's and Saturn's spin vectors. We show that Jupiter may have obtained its present obliquity by crossing of the s(8) resonance. This would set strict constraints on the character of migration during the early stage. Additional effects on Jupiter's obliquity are expected during the last gasp of migration when the s(7) resonance was approached. The magnitude of these effects depends on the precise value of the Jupiter's precession constant. Saturn's large obliquity was likely excited by capture into the s(8) resonance. This probably happened during the late stage of pl

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

2015

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

806

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

11

Strana od-do

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Kód UT WoS článku

000356810300143

EID výsledku v databázi Scopus

2-s2.0-84935013837