Calculating the structure of protoplanetary disks within the first few AU using Pisco

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dc.contributor.advisorLacy, John Howarden
dc.contributor.committeeMemberJaffe, Danen
dc.creatorHarrold, Samuel Thomasen
dc.date.accessioned2012-02-16T17:18:14Zen
dc.date.accessioned2017-05-11T22:24:27Z
dc.date.available2012-02-16T17:18:14Zen
dc.date.available2017-05-11T22:24:27Z
dc.date.issued2011-12en
dc.date.submittedDecember 2011en
dc.date.updated2012-02-16T17:18:31Zen
dc.descriptiontexten
dc.description.abstractThe calculation of the physical conditions near the inner rim of a protoplanetary disk using the new computational model Pisco is described. Diagnostic plots illustrate solutions for disk structure, radiation field, chemical composition, and heating and cooling of the disk in a steady-state approximation for both disks with unsettled dust and with settled dust. Disks with unsettled dust are found to have hotter gas temperatures above the disk photosphere and a more pronounced temperature inversion at the disk photosphere. Recommendations are made for the development of Pisco. Pisco has the potential to explore what observed molecular emission can imply about disk structure.en
dc.description.departmentAstronomyen
dc.format.mimetypeapplication/pdfen
dc.identifier.slug2152/ETD-UT-2011-12-4625en
dc.identifier.urihttp://hdl.handle.net/2152/ETD-UT-2011-12-4625en
dc.language.isoengen
dc.subjectProtoplanetary disken
dc.subjectRadiative transferen
dc.subjectAstrochemistryen
dc.subjectHeatingen
dc.subjectCoolingen
dc.titleCalculating the structure of protoplanetary disks within the first few AU using Piscoen
dc.type.genrethesisen

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