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Orbital Instability Zones of Space Balloons

Published online by Cambridge University Press:  12 April 2016

A. V. Krivov ,
L.L. Sokolov  and
J. Getino
A. V. Krivov
Affiliation:
Astronomical Institute, St. Petersburg UniversitySt. Petersburg, Russia
L.L. Sokolov
Affiliation:
Astronomical Institute, St. Petersburg UniversitySt. Petersburg, Russia
J. Getino
Affiliation:
Depto. de Matemàtica Aplicada Fund., Facultad de Ciencias Valladolid, Spain

Abstract

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We consider the motion of a spherically-symmetric balloon satellite perturbed by the Earth’s oblateness and solar radiation pressure. For equatorial satellite orbits and neglecting the Earth obliquity, the orbit-averaged equations for eccentricity and longitude of pericenter are integrable in quadratures (Krivov and Getino, 1996). The instability zone associated with the saddle separatrix in the phase space has been found and explored in depth. For semimajor axes about two Earth’s radii, and for area-to-mass ratios in the order of several tens cm2g−1, the amplitude and period of eccentricity oscillations may change nearly twofold under a small change of initial conditions or force parameters. We then restore the actual Earth obliquity of 235 and consider a spatial (non-integrable) problem. Near the saddle separatrix, a stochasticity zone appears that leads to large unpredictable eccentricity variations. The quasirandom motions of space balloons are investigated in terms of two-symbol (0-1) sequences by methods of stochastic celestial mechanics.

Type
Dynamics of Artificial Satellites and Space Debris
Information
International Astronomical Union Colloquium , Volume 165: Dynamics and Astrometry of Natural and Artificial Celestial Bodies , 1997 , pp. 361 - 366
Copyright
Copyright © Kluwer 1997

References

Hamilton, D.P. and Krivov, A.V.: 1996, “Circumplanetary dust dynamics: Effects of solar gravity, radiation pressure, planetary oblateness, and electromagnetism”, Icarus 123, 503–523.CrossRefGoogle Scholar
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