Results 111 to 120 of about 203 (129)

Free modes of layered oblate planets

Journal of Geophysical Research, 1963
The equations governing the motion of an elastic gravitating nonhomogeneous isotropic field are considered, and a general solution for the Laplace or Fourier transform of the displacement vector is given in spherical coordinates. The perturbation method is used to set the boundary conditions for an oblate layered spheroid and it is seen that, except ...
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Test Particle Motion around an Oblate Planet

Icarus, 1994
Abstract Ring flow kinematic features, such as, e.g., the shape of the narrow rings of Uranus or the streamlines of density waves of Saturn's rings, can be analyzed by fitting ring occultation data with m-lobe shapes with constant elements and constant precession rates. The orbital parameters thus obtained (e.g., the semimajor axis, the eccentricity)
Nicole Borderies-Rappaport, Pierre-Yves Longaretti   +1 more
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RISE AND SET TIME OF A SATELLITE ABOUT AN OBLATE PLANET

AIAA Journal, 1963
Summary: A technique is presented for the determination of the rise and set times of a satellite about an oblate planet. The solution depends on the ability to determine the rise and set eccentric anomalies from a single transcendental equation. The solution of the transcendental equation is facilitated greatly by an approximating technique.
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PERIODIC ORBITS ABOUT AN OBLATE PLANET

1963
Abstract : Periodic solutions of the equations of motion of a satellite of an oblate planet are investigated, using methods developed by Poincare (1892). The treatment covers both critical and non-critical angles.
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Relative Satellite Motion About an Oblate Planet

Journal of Guidance, Control, and Dynamics, 2002
A solution to the relative motion problem for satellites is constructed that is based on nearly circular reference periodic orbits and Floquet theory for the relative motion. This solution conceptually resembles the Clohessy-Wiltshire solution for relative motion, but includes all zonal harmonics of the Earth's gravitational field.
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Analytic Solution to the Relative Orbital Motion Around an Oblate Planet

AIAA Guidance, Navigation, and Control Conference, 2009
The paper offers a vectorial approach to the J2–perturbed relative orbital motion. The model uses mean orbital elements in order to derive closed form expressions for the relative position and relative velocity with respect to the LVLH frame attached on a main satellite.
Condurache, D., Martinusi, Vladimir
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Optimal Satellite Formation Establishment about an Oblate Planet

AIAA Guidance, Navigation, and Control Conference, 2011
This paper suggests a new approach for generating bounded motion between two spacecraft orbiting an oblate planet. As opposed to most works, the suggested approach does not rely on averaging the osculating orbital elements. Instead, the problem is formulated in local-vertical local-horizontal coordinates, without approximating the gravitational ...
Vladimir Martinusi, Pini Gurfil
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Perturbation of a satellite orbiter by the oblateness of the primary planet

Celestial Mechanics, 1976
The perturbation of an orbiter around a large satellite of a giant planet (Jupiter, Saturn, Uranus or Neptune) produced by the oblateness of the planet is investigated. The perturbing force of theJ2-term (general case) and theJ4-term (special case of small eccentricity and inclination) is expanded in an appropriate form and the main term and the ...
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Perturbations by the oblateness of the Earth and by the planets in the motion of the Moon

Celestial Mechanics, 1982
Perturbations in the motion of the Moon are computed for the effect by the oblateness of the Earth and for the indirect effect of planets. Based on Delaunay's analytical solution of the main problem, the computations are performed by a method of Fourier series operation.
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Nonlinear theory of secular perturbations of satellites of an oblate planet

Astronomy Letters, 2012
Anonlinear analytical theory of secular perturbations in the problem of the motion of a systemof small bodies around a major attractive center has been developed. Themutual perturbations of the satellites and the influence of the oblateness of the central body are taken into account in the model.
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