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dc.contributor.advisorChairperson, Graduate Committee: Dana W. Longcope.en
dc.contributor.authorMalanushenko, Anna Viktorovnaen
dc.coverage.spatialSunen
dc.date.accessioned2013-06-25T18:43:00Z
dc.date.available2013-06-25T18:43:00Z
dc.date.issued2010en
dc.identifier.urihttps://scholarworks.montana.edu/xmlui/handle/1/1780
dc.description.abstractTwist of magnetic field is believed to play important role in driving instabilities that result in eruptive events on the Sun. This thesis provides different methods to measure twist in the solar corona. First, given a model of coronal field, twist of a magnetic domain (i.e., a volume that contains all field lines connecting two regions of interest in the photosphere) is well studied for cases when the domain is a thin cylinder. For cases when such approximation is inapplicable a generalization of twist can be derived from a quantity called additive self-helicity. I develop explicit numerical methods to compute generalized twist. I also demonstrate that such a quantity sets a threshold on kink instability like the traditional twist does for thin cylinders. In a more realistic scenario, coronal magnetic field is not known and so neither is its helicity. There are two principal methods to overcome this problem. The first is to integrate helicity flux across the photosphere (as helicity is believed to be approximately conserved in the corona) using magnetic field on Sun's surface. There is little published evidence as yet that coronal helicity indeed corresponds to its integrated photospheric flux. The second is to extrapolate the coronal magnetic field using surface measurements as boundary conditions and use this extrapolation for helicity computation; for fields with complicated structure such extrapolations are extremely challenging and suffer from major drawbacks. I develop a method to estimate twist of coronal fields without attempting complicated extrapolations or studying helicity flux. The method builds a simple uniformly-twisted magnetic field and adjusts its properties until there is one line in this field that matches one coronal loop; this is repeated for all evident coronal loops resulting in twist measurements for each individual loop. I use this method to demonstrate that the rate of change of twist in the solar corona is indeed approximately equal to the one derived from photospheric helicity flux. The results of this dissertation are useful for better understanding of magnetic topology in general. They are also extremely promising for extrapolating coronal magnetic fields. Measurements of coronal twist might aid in predicting magnetic instabilities.en
dc.language.isoengen
dc.publisherMontana State University - Bozeman, College of Letters & Scienceen
dc.subject.lcshMagnetic fields.en
dc.subject.lcshTopology.en
dc.titleTwist in coronal magnetic fields
dc.typeDissertation
dc.rights.holderCopyright Anna Viktorovna Malanushenko 2010en
thesis.catalog.ckey1522506en
thesis.degree.committeemembersMembers, Graduate Committee: Charles Kankelborg; David McKenzie; Jiong Qiu; Petrus Martens; Valerie Copieen
thesis.degree.departmentPhysics.en
thesis.degree.genreDissertationen
thesis.degree.namePhDen
thesis.format.extentfirstpage1en
thesis.format.extentlastpage159en
mus.identifier.categoryPhysics & Mathematics
mus.relation.departmentPhysics.en_US
mus.relation.universityMontana State University - Bozemanen_US


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