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dc.contributor.author Michael, Scott
dc.date.accessioned 2011-02-18T13:17:35Z
dc.date.available 2011-02-18T13:17:35Z
dc.date.issued 2011-02-18
dc.identifier.uri http://hdl.handle.net/2022/12960
dc.description In the External Files area below, links to the streaming video versions of the data files are available. This list explains the correlation of the VAC streaming video name with the data file title: 0.3JUP10ORP=VAC0930; 1JUP0ORP=VAC0931; 3JUP0ORP=VAC0932; BASELINE=VAC0933; 1JUP10ORP=VAC0934; 3JUP10ORP=VAC0935; 0.3JUP0ORP=VAC0936
dc.description Note: The version of the dissertation attached to this record is the author's final version and not the Indiana University official version of record. At a future date, when we have the IU version, we will update this note with a link to that version.
dc.description.abstract The study of gravitational instabilities (GIs) and their effects in protoplanetary disks has been an area of active research for over a decade. Although some studies have indicated that GIs cannot form gas giant planets directly, it is clear that they can have a significant effect on a protoplanetary disk. In this dissertation I present several areas where GIs may play a key role in the evolution of a protoplanetary disk. These studies are carried out using three dimensional numerical simulations. I have carried out and analyzed nearly twenty simulations with varying initial conditions, resolutions, and physical effects. Although all indications from these simulations are that GIs cannot form gas giant planets directly at radii smaller than 40 AU, they have shown that GIs can have a dramatic effect on protoplanetary disk structure and planets embedded in a protoplanetary disk. I present several key results including: the effects of a varied initial surface density profile azimuthal resolution, the amplitude of the initial random perturbation, and the adiabatic index used on the onset, strength and general evolution of GIs in protoplanetary disks. Additionally, I present results on studies of the interaction of the instabilities with the central star when it is allowed to move freely in response to the action of the GIs. Finally, I present several results regarding the interaction of embedded massive planets and GI active disks. I find that the presence of massive planets can have a dramatic effect on the evolution of GIs in an active disk, and the GIs can also dramatically effect them migration of the embedded planet. In fact, the action of the GIs may planets to migrate outward, contrary to the standard theory of the planet migration in laminar disks. en
dc.publisher Indiana University en
dc.relation.uri http://purl.dlib.indiana.edu/iudl/general/video/VAC0932
dc.relation.uri http://purl.dlib.indiana.edu/iudl/general/video/VAC0936
dc.relation.uri http://purl.dlib.indiana.edu/iudl/general/video/VAC0934
dc.relation.uri http://purl.dlib.indiana.edu/iudl/general/video/VAC0931
dc.relation.uri http://purl.dlib.indiana.edu/iudl/general/video/VAC0935
dc.relation.uri http://purl.dlib.indiana.edu/iudl/general/video/VAC0933
dc.relation.uri http://purl.dlib.indiana.edu/iudl/general/video/VAC0930
dc.subject gravitational instabilities en
dc.subject astrophysics en
dc.title Planet Migration Induced by Gravitational Instabilities en
dc.type Other en


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