Show simple item record

dc.contributor.advisorChairperson, Graduate Committee: Sachiko Tsuruta.en
dc.contributor.authorLiebmann, Andrew Cargill.en
dc.date.accessioned2013-06-25T18:36:54Z
dc.date.available2013-06-25T18:36:54Z
dc.date.issued2010en
dc.identifier.urihttps://scholarworks.montana.edu/xmlui/handle/1/1730
dc.description.abstractPresented is the detailed analysis of three Narrow Line Seyfert 1 galaxies using the method of dynamical spectral analysis. These are NGC 4051, IRAS F12397+3333 and Mrk 766. The highly variable NGC 4051 exhibits some dramatic changes over the course of two observations. These dramatic changes are attributed to a variable emission region being partially covered by a fixed, thick absorbing cloud. A unique time region was found where the emission region becomes smaller than the absorbing cloud. Source enters a true minimal phase and appears quite stable, appearing to "turn off." When in its lowest flux states NGC 4051 has a thermal plasma feature suggesting starburst activity in the nucleus. The possibility of starburst activity proves an important link in the understanding of the evolution of Active Galactic Nuclei. IRAS F12397+3333, a little studied source, was found to possess a complex, dusty, warm absorber spectrum of helium- and hydrogen-like carbon, nitrogen, oxygen, neon and several ionic species of iron. This is similar to the spectrum of IRAS 13349+2348. A two-phase gas was used to model this spectrum. The location of the gas is consistent with being located in the narrow line region. Two types of variability were found in the rapidly varying Mrk 766. The longterm variability and its associated spectral flattening seen in two observations are caused by a thick partially covering cloud and variable emission region. However the average spectral behavior shows partial covering of a thinner cloud. The result is a "lumpy cloud." When the source is dim a thicker portion of the clouds covers it, but as the source brightens and enlarges the thinner portion plays a more dominant role in the covering. The short, rapid variability is caused by the combination of a highly variable power law component and a stable reflected component, referred to here as ionized relativistic reflection. Finally, some unique flares were discovered. Unlike the other flares seen in the lightcurves, these occur only in the 0.3-2.0 keV band. They are attributed as a 'hot spot' on the accretion disk.en
dc.language.isoengen
dc.publisherMontana State University - Bozeman, College of Letters & Scienceen
dc.subject.lcshActive galaxies.en
dc.subject.lcshSeyfert galaxies.en
dc.subject.lcshX-rays.en
dc.titleTemporal and dynamical spectral analysis of select narrow line Seyfert 1 galaxies
dc.typeDissertation
dc.rights.holderCopyright Andrew Cargill Liebmann 2010en
thesis.catalog.ckey1606752en
thesis.degree.committeemembersMembers, Graduate Committee: Neil J. Cornish; Petrus Martens; John L. Carlsten; Charles Kankelborgen
thesis.degree.departmentPhysics.en
thesis.degree.genreDissertationen
thesis.degree.namePhDen
thesis.format.extentfirstpage1en
thesis.format.extentlastpage187en
mus.identifier.categoryPhysics & Mathematics
mus.relation.departmentPhysics.en_US
mus.relation.universityMontana State University - Bozemanen_US


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record