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dc.contributor.authorEberle, William Jasonen_US
dc.date.accessioned2007-08-23T01:56:24Z
dc.date.available2007-08-23T01:56:24Z
dc.date.issued2007-08-23T01:56:24Z
dc.date.submittedMay 2007en_US
dc.identifier.otherDISS-1685en_US
dc.identifier.urihttp://hdl.handle.net/10106/279
dc.description.abstractIn this thesis, the onset of instability for a planet which is part of a stellar binary system is investigated by running numerical simulations of the circular restricted three body problem. This study also makes use of a rotating (synodic) coordinate system keeping both binary stars at rest. This allows the definition of a constant of motion (Jacobi's constant), which in turn sets a permissible region of motion for the planet. As the initial conditions are varied, the boundary of the permissible region of motion passes through each of the three collinear equilibrium points with significant changes to the orbit of the planet at or near each crossing. The average eccentricity of the orbit serves as an additional means of determining the stability. The stability limits obtained via these methods agree with other methods that were obtained with simulations over much longer time intervals.en_US
dc.description.sponsorshipCuntz, Manfreden_US
dc.language.isoENen_US
dc.publisherPhysicsen_US
dc.titleCase Studies Of The Circular Restricted Three Body Problemen_US
dc.typeM.S.en_US
dc.contributor.committeeChairCuntz, Manfreden_US
dc.degree.departmentPhysicsen_US
dc.degree.disciplinePhysicsen_US
dc.degree.grantorUniversity of Texas at Arlingtonen_US
dc.degree.levelmastersen_US
dc.degree.nameM.S.en_US
dc.identifier.externalLinkhttps://www.uta.edu/ra/real/editprofile.php?onlyview=1&pid=110
dc.identifier.externalLinkDescriptionLink to Research Profiles


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