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• W208080319 abstract "Most of the discovered extrasolar planets are massive, Jupitersized bodies, moving about their central stars along considerably eccentric orbits. Low-mass planets like the Earth still cannot be observed in these systems. However, their existence is especially interesting in view of the search for extraterrestrial life as well as planetary formation theories. In this work, we examine the orbital stability of low-mass planets in the systems with “Jupiters” on eccentric orbits, in the frame of restricted elliptical three-body problem. The initial orbit of the massless particle representing an Earth-sized planet is circular. The regions of regular and chaotic motion are studied, a simple analytical model of the regular motion is presented. If the distance between the orbits of “Jupiter” and massless particle is sufficiently small, the motion becomes chaotic. In the transition region between the regularity and chaos the trajectory properties are highly sensitive to the initial positions of planets on their orbits. These trajectories are investigated in more detail. In contrast to the region of regular motion, we found that low-eccentricity orbits exist in the transition region, some of which are stable on the time scale of 10 orbital revolutions of “Jupiter.” The discovery of extrasolar planetary systems is an outstanding achivement of science. Many new problems connected with extrasolar planets arise in astronomy. For example, new planetary systems differ sufficiently from the Solar system, and known theories of planet formation cannot explain formation of the extrasolar planets. Now we will discuss one dynamical problem. Many massive extrasolar planets have large orbital eccentricities, in contrast to Jupiter (Schneider 2003). We cannot observe low-mass planets like the Earth or Mars. The problem considered in this paper is the influence of the massive planet with the large orbital eccentricity on possible motions of small planets. What can we say about planetary system design, if extrasolar “Jupiter” has a large orbital eccentricity? In particular, the existence of quasi-circular orbits of small planets like the Earth is very interesting. We constrain ourselves to model planetary systems similar to the solar system. The mass of the star is equal to the solar mass, semi-major axis of “Jovian” orbit is equal to 5.2 A.U., the low-mass planet has initially circular orbit. The only difference is a large eccentricity of Jovian orbit. We investigate the low-mass planet motion within the framework of the restricted elliptical three-body problem. The consideration has been done for the planar problem, but if the inclination is small, our results hold true. We discuss mainly the “outer” problem, for which the distance between the star and the low-mass planet is longer than between a star and a massive planet. The results have been derived numerically; in order to verify them, we use different independent program tools, as well as analytical tools." @default.
• W208080319 created "2016-06-24" @default.
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• W208080319 date "2004-11-01" @default.
• W208080319 modified "2023-09-23" @default.
• W208080319 title "Motions in Extrasolar Planetary System: between Regularity and Chaos" @default.
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