Influence of periodic orbits on the formation of giant planetary systems

Résultats de recherche: Contribution à un journal/une revueArticle

Résumé

The late-stage formation of giant planetary systems is rich in interesting dynamical mechanisms. Previous simulations of three giant planets initially on quasi-circular and quasi-coplanar orbits in the gas disc have shown that highly mutually inclined configurations can be formed, despite the strong eccentricity and inclination damping exerted by the disc. Much attention has been directed to inclination-type resonance, asking for large eccentricities to be acquired during the migration of the planets. Here we show that inclination excitation is also present at small to moderate eccentricities in two-planet systems that have previously experienced an ejection or a merging and are close to resonant commensurabilities at the end of the gas phase. We perform a dynamical analysis of these planetary systems, guided by the computation of planar families of periodic orbits and the bifurcation of families of spatial periodic orbits. We show that inclination excitation at small to moderate eccentricities can be produced by (temporary) capture in inclination-type resonance and the possible proximity of the non-coplanar systems to spatial periodic orbits contributes to maintaining their mutual inclination over long periods of time.

langue originaleAnglais
Numéro d'article19
journalCelestial Mechanics and Dynamical Astronomy
Volume130
Numéro de publication2
Les DOIs
étatPublié - 1 févr. 2018

Empreinte digitale

planetary systems
Inclination
eccentricity
Periodic Orbits
inclination
Orbits
Planets
Eccentricity
orbits
planet
planets
bifurcation
Excitation
Gases
Merging
gas
damping
Coplanar
Damping
Inclined

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title = "Influence of periodic orbits on the formation of giant planetary systems",
abstract = "The late-stage formation of giant planetary systems is rich in interesting dynamical mechanisms. Previous simulations of three giant planets initially on quasi-circular and quasi-coplanar orbits in the gas disc have shown that highly mutually inclined configurations can be formed, despite the strong eccentricity and inclination damping exerted by the disc. Much attention has been directed to inclination-type resonance, asking for large eccentricities to be acquired during the migration of the planets. Here we show that inclination excitation is also present at small to moderate eccentricities in two-planet systems that have previously experienced an ejection or a merging and are close to resonant commensurabilities at the end of the gas phase. We perform a dynamical analysis of these planetary systems, guided by the computation of planar families of periodic orbits and the bifurcation of families of spatial periodic orbits. We show that inclination excitation at small to moderate eccentricities can be produced by (temporary) capture in inclination-type resonance and the possible proximity of the non-coplanar systems to spatial periodic orbits contributes to maintaining their mutual inclination over long periods of time.",
keywords = "Formation of planetary systems, Inclination-type resonance, Periodic orbits, Planet-disc interactions",
author = "Libert, {Anne Sophie} and Sotiris Sotiriadis and Antoniadou, {Kyriaki I.}",
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Influence of periodic orbits on the formation of giant planetary systems. / Libert, Anne Sophie; Sotiriadis, Sotiris; Antoniadou, Kyriaki I.

Dans: Celestial Mechanics and Dynamical Astronomy, Vol 130, Numéro 2, 19, 01.02.2018.

Résultats de recherche: Contribution à un journal/une revueArticle

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T1 - Influence of periodic orbits on the formation of giant planetary systems

AU - Libert, Anne Sophie

AU - Sotiriadis, Sotiris

AU - Antoniadou, Kyriaki I.

PY - 2018/2/1

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N2 - The late-stage formation of giant planetary systems is rich in interesting dynamical mechanisms. Previous simulations of three giant planets initially on quasi-circular and quasi-coplanar orbits in the gas disc have shown that highly mutually inclined configurations can be formed, despite the strong eccentricity and inclination damping exerted by the disc. Much attention has been directed to inclination-type resonance, asking for large eccentricities to be acquired during the migration of the planets. Here we show that inclination excitation is also present at small to moderate eccentricities in two-planet systems that have previously experienced an ejection or a merging and are close to resonant commensurabilities at the end of the gas phase. We perform a dynamical analysis of these planetary systems, guided by the computation of planar families of periodic orbits and the bifurcation of families of spatial periodic orbits. We show that inclination excitation at small to moderate eccentricities can be produced by (temporary) capture in inclination-type resonance and the possible proximity of the non-coplanar systems to spatial periodic orbits contributes to maintaining their mutual inclination over long periods of time.

AB - The late-stage formation of giant planetary systems is rich in interesting dynamical mechanisms. Previous simulations of three giant planets initially on quasi-circular and quasi-coplanar orbits in the gas disc have shown that highly mutually inclined configurations can be formed, despite the strong eccentricity and inclination damping exerted by the disc. Much attention has been directed to inclination-type resonance, asking for large eccentricities to be acquired during the migration of the planets. Here we show that inclination excitation is also present at small to moderate eccentricities in two-planet systems that have previously experienced an ejection or a merging and are close to resonant commensurabilities at the end of the gas phase. We perform a dynamical analysis of these planetary systems, guided by the computation of planar families of periodic orbits and the bifurcation of families of spatial periodic orbits. We show that inclination excitation at small to moderate eccentricities can be produced by (temporary) capture in inclination-type resonance and the possible proximity of the non-coplanar systems to spatial periodic orbits contributes to maintaining their mutual inclination over long periods of time.

KW - Formation of planetary systems

KW - Inclination-type resonance

KW - Periodic orbits

KW - Planet-disc interactions

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