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dc.contributor.advisorChairperson, Graduate Committee: David E. McKenzieen
dc.contributor.authorFreed, Michael Scott.en
dc.contributor.otherDana W. Longcope and David E. McKenzie were co-authors of the article, 'Three-year global survey of coronal null points from PFSS modeling and SDO observations' in the journal 'Solar physics' which is contained within this thesis.en
dc.contributor.otherDavid E. McKenzie, Dana W. Longcope, and Mikki Wilburn were co-authors of the article, 'Analysis of flows inside quiescent prominences as captured by hinode/solar optical telescope' in the journal 'The astrophysical journal' which is contained within this thesis.en
dc.contributor.otherDavid E. McKenzie was a co-author of the article, 'Quantifying turbulent dynamics found within the plasma sheets of multiple solar flares' submitted to the journal 'The astrophysical journal' which is contained within this thesis.en
dc.coverage.spatialSun Coronaen
dc.coverage.spatialSun Prominencesen
dc.date.accessioned2016-10-27T15:37:31Z
dc.date.available2016-10-27T15:37:31Z
dc.date.issued2016en
dc.identifier.urihttps://scholarworks.montana.edu/xmlui/handle/1/9771
dc.description.abstractSolar observations were employed in this work to quantify motion and structures seen in the sun's corona with particular attention given to features found at the solar limb. These features consist of coronal magnetic-null points, quiescent prominences, and post flare eruption plasma sheets. Extreme-ultraviolet (EUV) observations from the Solar Dynamics Observatory (SDO) spacecraft were used to determine the fidelity of the commonly used potential field source surface (PFSS) model for predicting the location of coronal magnetic-null-points. Several properties of the null points were also investigated to ascertain if they had any effect on their observability. Next, quiescent prominence observations from the Hinode/Solar Optical Telescope satellite were used to create velocity maps of the plasma found in these structures. The derived velocities provided insight into the vorticity, kinetic energy, and oscillations that reside in these prominences. Primarily, this investigation was concerned with determining the distribution of velocity and vorticity at different length scales by applying a power spectral density analysis. All of this information is intended to strengthen our understanding on how these prominences evolve and potentially become unstable. An identical analysis is then conducted on post-flare-eruption plasma sheets observed in EUV by the space based SDO and TRACE satellites. Investigating the dynamics that reside in these plasma sheets are crucial for understanding the conditions that trigger and accelerate the magnetic reconnection responsible for producing these energetic solar flares.en
dc.language.isoenen
dc.publisherMontana State University - Bozeman, College of Letters & Scienceen
dc.subject.lcshFluid dynamics.en
dc.subject.lcshMagnetic reconnection.en
dc.subject.lcshObservation (Scientific method).en
dc.titleAn empirical study of coronal observations at the solar limben
dc.typeDissertationen
dc.rights.holderCopyright 2016 by Michael Scott Freed.en
thesis.catalog.ckey3149306en
thesis.degree.committeemembersMembers, Graduate Committee: David E. McKenzie (chairperson); Jiong Qiu; Dana W. Longcope; Greg Francis; John L. Carlsten.en
thesis.degree.departmentPhysics.en
thesis.degree.genreDissertationen
thesis.degree.namePhDen
thesis.format.extentfirstpage1en
thesis.format.extentlastpage205en
mus.identifier.categoryPhysics & Mathematicsen_US
mus.relation.universityMontana State University - Bozemanen_US
mus.data.thumbpage85


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