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Qualitatively similar orbits are obtained in the many par ticle calculations.
In opposition to this, chaos is effective for causing rapid desynchronization, because of its characteristic exponential divergence of nearby orbits.
Dynamically we find most orbits to be stable over long time scales and typically this happens in a wider parameter area than in co-rotating systems.
The bar will hence be able to relocate stars, and stars with low or high metallicity could be found far away from their original orbits.
We only need that the return maps at periodic orbits are diagonal on the stable and unstable manifolds.
In most cases, those planets follow orbits with significant eccentricity, leading to substantial seasonal temperature excursions.
In most cases, those planets follow orbits with significant eccentricity, leading to substantial temperature excursions.
Indeed, nebular drag and collisions would ensure that orbits with zero eccentricity were preferred.
The steady-state solution of the equation of motion is then derived in cartesian coordinates and two groups of electron orbits are defined.
Here, a planetary system consisting of one star and two identical-mass planets in circular but mutually inclined orbits is considered.
Quasiperiodic orbits can look quite complicated, especially if there exist many incommensurable frequencies.
The velocity of the planet orbiting at this distance satisfies the relation vn=w/n.
The project mission was to locate intelligent signals coming from hypothetical planets orbiting the stars.
A caustic is formed by the envelope of these orbits.
Note that the orbits are almost per fectly laminar and there is no sign of filamentation.
