Dynamical evolution of the restricted elliptic planetary three-body problem

Research output

Abstract

Today (15.05.08) we have 288 exoplanets, 25 multisystems (Schneider, 2008). Most of the discovered extrasolar planets are massive, Jupiter-sized bodies, moving around their host stars along considerably eccentric orbits. Low-mass planets like the Earth cannot still be observed in these systems. There are many mean-motion resonances in the known extrasolar planetary systems. We investigate the low-mass exoplanet possible motions within the framework of the restricted elliptical three-body problem using numerical and analytical tools. Especially interesting is the possibility of near-circular motions in the habitability zones – regions near the star, where the physical conditions are favourable for liquid water existence. Near-circular orbits in the habitability zones are favour for highly evolved matter.
Original languageEnglish
Title of host publicationResonances, stabilization, and stable chaos in hierarchical triple systems, 2008, p.61-70
Pages61-70
Publication statusPublished - 2008

Fingerprint

three body problem
extrasolar planets
habitability
stars
eccentric orbits
planetary systems
circular orbits
Jupiter (planet)
planets
liquids
water

Cite this

Sokolov, L., Pitjev, N., & Eskin, B. (2008). Dynamical evolution of the restricted elliptic planetary three-body problem. In Resonances, stabilization, and stable chaos in hierarchical triple systems, 2008, p.61-70 (pp. 61-70)
Sokolov, L. ; Pitjev, N. ; Eskin, B. / Dynamical evolution of the restricted elliptic planetary three-body problem. Resonances, stabilization, and stable chaos in hierarchical triple systems, 2008, p.61-70. 2008. pp. 61-70
@inbook{89209b579c6d4530bf7984030497d0b6,
title = "Dynamical evolution of the restricted elliptic planetary three-body problem",
abstract = "Today (15.05.08) we have 288 exoplanets, 25 multisystems (Schneider, 2008). Most of the discovered extrasolar planets are massive, Jupiter-sized bodies, moving around their host stars along considerably eccentric orbits. Low-mass planets like the Earth cannot still be observed in these systems. There are many mean-motion resonances in the known extrasolar planetary systems. We investigate the low-mass exoplanet possible motions within the framework of the restricted elliptical three-body problem using numerical and analytical tools. Especially interesting is the possibility of near-circular motions in the habitability zones – regions near the star, where the physical conditions are favourable for liquid water existence. Near-circular orbits in the habitability zones are favour for highly evolved matter.",
author = "L. Sokolov and N. Pitjev and B. Eskin",
year = "2008",
language = "English",
isbn = "978-5-9651-0295-2",
pages = "61--70",
booktitle = "Resonances, stabilization, and stable chaos in hierarchical triple systems, 2008, p.61-70",

}

Sokolov, L, Pitjev, N & Eskin, B 2008, Dynamical evolution of the restricted elliptic planetary three-body problem. in Resonances, stabilization, and stable chaos in hierarchical triple systems, 2008, p.61-70. pp. 61-70.

Dynamical evolution of the restricted elliptic planetary three-body problem. / Sokolov, L.; Pitjev, N.; Eskin, B.

Resonances, stabilization, and stable chaos in hierarchical triple systems, 2008, p.61-70. 2008. p. 61-70.

Research output

TY - CHAP

T1 - Dynamical evolution of the restricted elliptic planetary three-body problem

AU - Sokolov, L.

AU - Pitjev, N.

AU - Eskin, B.

PY - 2008

Y1 - 2008

N2 - Today (15.05.08) we have 288 exoplanets, 25 multisystems (Schneider, 2008). Most of the discovered extrasolar planets are massive, Jupiter-sized bodies, moving around their host stars along considerably eccentric orbits. Low-mass planets like the Earth cannot still be observed in these systems. There are many mean-motion resonances in the known extrasolar planetary systems. We investigate the low-mass exoplanet possible motions within the framework of the restricted elliptical three-body problem using numerical and analytical tools. Especially interesting is the possibility of near-circular motions in the habitability zones – regions near the star, where the physical conditions are favourable for liquid water existence. Near-circular orbits in the habitability zones are favour for highly evolved matter.

AB - Today (15.05.08) we have 288 exoplanets, 25 multisystems (Schneider, 2008). Most of the discovered extrasolar planets are massive, Jupiter-sized bodies, moving around their host stars along considerably eccentric orbits. Low-mass planets like the Earth cannot still be observed in these systems. There are many mean-motion resonances in the known extrasolar planetary systems. We investigate the low-mass exoplanet possible motions within the framework of the restricted elliptical three-body problem using numerical and analytical tools. Especially interesting is the possibility of near-circular motions in the habitability zones – regions near the star, where the physical conditions are favourable for liquid water existence. Near-circular orbits in the habitability zones are favour for highly evolved matter.

M3 - Article in an anthology

SN - 978-5-9651-0295-2

SP - 61

EP - 70

BT - Resonances, stabilization, and stable chaos in hierarchical triple systems, 2008, p.61-70

ER -

Sokolov L, Pitjev N, Eskin B. Dynamical evolution of the restricted elliptic planetary three-body problem. In Resonances, stabilization, and stable chaos in hierarchical triple systems, 2008, p.61-70. 2008. p. 61-70