Periodic solutions and their parametric evolution in the planar case of the (n + 1) ring problem with oblateness

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dc.contributor.author Elipe, A en
dc.contributor.author Arribas, M en
dc.contributor.author Kalvouridis, TJ en
dc.date.accessioned 2014-03-01T02:50:51Z
dc.date.available 2014-03-01T02:50:51Z
dc.date.issued 2006 en
dc.identifier.uri http://hdl.handle.net/123456789/35159
dc.relation.uri http://www.scopus.com/inward/record.url?eid=2-s2.0-33845989815&partnerID=40&md5=2a77940c263b0093d6af5105f84d9ada en
dc.subject.other Angular velocity en
dc.subject.other Periodic orbits en
dc.subject.other Radiation sources en
dc.subject.other Ring problem en
dc.subject.other Bifurcation (mathematics) en
dc.subject.other Elementary particles en
dc.subject.other Gravitational effects en
dc.subject.other Parameter estimation en
dc.subject.other Radiation effects en
dc.subject.other Velocity measurement en
dc.subject.other Space flight en
dc.title Periodic solutions and their parametric evolution in the planar case of the (n + 1) ring problem with oblateness en
heal.type conferenceItem en
heal.publicationDate 2006 en
heal.abstract In the N- body ring problem, the motion of an infinitesimal particle attracted by the gravitational field of (n + 1) bodies is studied. These bodies are arranged in a planar ring configuration. This configuration consists of n primaries of equal mass m located at the vertices of a regular polygon that is rotating on its own plane about its center of mass with a constant angular velocity w. Another primary of mass m0 = βm (β ≥ 0 parameter) is placed at the center of the ring. More over, in this paper we assume that the central body may be an ellipsoid, or a radiation source, which introduces a new parameter ε. For this case, since the number of equilibria and bifurcations is different from the classical problem, the dynamics is much richer. In this paper, we find families of periodic orbits, and make an analysis of the orbits by studying their evolution and stability along the family for several values of the new parameter introduced. Copyright © 2006 by the American Institute of Aeronautics and Astronautics, Inc. All rights reserved. en
heal.journalName Collection of Technical Papers - AIAA/AAS Astrodynamics Specialist Conference, 2006 en
dc.identifier.volume 3 en
dc.identifier.spage 1898 en
dc.identifier.epage 1914 en

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