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 -