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- W2147020909 abstract "We present the exact solutions in three dimensions for the orbital elements of a satellite particle continuously exposed to weak solar radiation. The solutions are obtained from a set of auxiliary variables, which are separable and therefore integrable. We have illustrated various examples of the behavior of the elements as they evolve cyclically. In addition, there are three items worthy of note: (1) The planar case, wherein the orbital plane contains the Sun, has been solved previously; but here a near-planar orbit is shown to evolve away from its original, nearly planar orientation. This consequence of radiation pressure may be contrasted with gravitational perturbation by massive bodies in the orbital plane, which tend to stabilize such orbits. (2) In the general, three-dimensional case the orbital elements not only have components that vary with time, as expected, in a uniform sinusoidal manner. They possess, as well, nonuniform sinusoidal variations that have the same period as the uniform variations. (3) The semimajor axis, a, which is related to the total energy, may be regarded as constant in the first order, on the grounds that a particle returns essentially to its starting point after one orbit. Here we derive the actual time variation of a from the extended Laplace constant. That constant was obtained in Paper I from the separation of variables that is allowed when the perturbed Keplerian problem is formulated in parabolic coordinates, and it remains a valid constant even when the total Keplerian energy is not. The relative amplitude, Δa(t)/a(0) varies as (a/rx)4, where rx is the distance from the planet where the gravitational and radiative acceleration are equal (i.e., the radius of the exosphere). Hence, the variation in a(t) is very small, except for orbits comparable in size to the exosphere itself." @default.
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- W2147020909 date "1993-12-01" @default.
- W2147020909 modified "2023-10-14" @default.
- W2147020909 title "Radiation Pressure Dynamics in Planetary Exospheres II. Closed Solutions for the Evolution of Orbital Elements" @default.
- W2147020909 doi "https://doi.org/10.1006/icar.1993.1182" @default.
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