Modelling dusty planetary disks using secular perturbation theory

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dc.contributor.advisor Hahn, Joseph Michael
dc.creator Capobianco, Christopher Claudio 2011-05-09T12:32:02Z 2011-05-09T12:32:02Z 2006
dc.identifier.other QB792 C37 2006
dc.description ix, 91 leaves : ill. (some col.) ; 29 cm.
dc.description Includes abstract and appendices.
dc.description Includes bibliographical references (leaves 86-91).
dc.description.abstract Optical coronagraphic imaging of the circumstellar dust disk around β Pictoris reveals that the inner portion of the disk is warped, and this warp is typically attributed to the presence of a planetary system. Mouillet et al . (1997b) argue the warp is the result of a single planet on an inclined orbit, but the warp in their models are an artifact of their unphysical initial conditions. Using a more realistic set of initial conditions, at least two planets on mutually inclined orbits are required to produce the observed warp. The goal of this research is to find the two-planet configuration that best describes the warp in β Pictoris, using the more realistic set of initial conditions. This is accomplished via a parameter survey, where it is found that a ∼ 7 M J planet at 35 AU and a ∼ 3 M J planet at 131 AU, both on nearly circular orbits and inclined ∼ 2° to the disk mid-plane are able to accurately reproduce the observed warp in the β Pictoris disk.
dc.description.provenance Made available in DSpace on 2011-05-09T12:32:02Z (GMT). No. of bitstreams: 0 en
dc.language.iso en
dc.publisher Halifax, N.S. : Saint Mary's University
dc.subject.lcc QB792
dc.subject.lcsh Circumstellar matter
dc.subject.lcsh Perturbation (Astronomy)
dc.subject.lcsh Stellar dynamics
dc.subject.lcsh Dwarf stars
dc.subject.lcsh Extrasolar planets
dc.title Modelling dusty planetary disks using secular perturbation theory
dc.type Text Master of Science in Astronomy Masters Astronomy and Physics Saint Mary's University (Halifax, N.S.)
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