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dc.contributor.authorCampanella, Giammarco
dc.date.accessioned2015-09-01T14:04:14Z
dc.date.available2015-09-01T14:04:14Z
dc.date.issued2013-06
dc.identifier.citationCampanella, G. 2013. Dynamical Aspects of Exoplanetary Systems. Queen Mary University of London.en_US
dc.identifier.urihttp://qmro.qmul.ac.uk/xmlui/handle/123456789/8374
dc.descriptionPhDen_US
dc.description.abstractThe detection of more than 130 multiple planet systems makes it necessary to interpret a broader range of properties than are shown by our Solar system. This thesis covers aspects linked to the proliferation in recent years of multiple extrasolar planet systems. A narrow observational window, only partially covering the longest orbital period, can lead to solutions representing unrealistic scenarios. The best-fit solution for the three-planet extrasolar system of HD 181433 describes a highly unstable configuration. Taking into account the dynamical stability as an additional observable while interpreting the RV data, I have analysed the phase space in the neighbourhood of the statistical best-fit. The two giant companions are found to be locked in the 5:2 MMR in the stable best-fit model. I have analysed the dynamics of the system HD 181433 by assessing different scenarios that may explain the origin of these eccentric orbits, with particular focus on the innermost body. A scenario is considered in which the system previously contained an additional giant planet that was ejected during a period of dynamical instability among the planets. Also considered is a scenario in which the spin-down of the central star causes the system to pass through secular resonance. In its simplest form this latter scenario fails to produce the system observed. If additional short-period low mass planets are present in the system, I find that mutual scattering can release planet b from the secular resonance, leading to a system with orbital parameters similar to those observed today. Finally, I have studied the evolution of low mass planets interacting with a gas-giant planet embedded in a gaseous disc. The transit timing method allows the detection of non-transiting planets through their gravitational perturbations. I have investigated the detectability of low mass planets neighbouring short-period giants after protoplanetary disc dispersal.en_US
dc.language.isoenen_US
dc.publisherQueen Mary University of Londonen_US
dc.subjectAstronomyen_US
dc.subjectPlanetsen_US
dc.titleDynamical Aspects of Exoplanetary Systemsen_US
dc.typeThesisen_US
dc.rights.holderThe copyright of this thesis rests with the author and no quotation from it or information derived from it may be published without the prior written consent of the author


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    Theses Awarded by Queen Mary University of London

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