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• W337054967 abstract "This thesis presents an examination of a range of dynamic phenomena present throughout thesolar atmosphere, from the photosphere to the corona. Above the photosphere, where theplasma fi is small, the emitting plasma structure and dynamics are tied intimately to the solarmagnetic field.Firstly, a wavelet analysis is applied to multi-temperature spectroscopic data observingnetwork-internetwork regions across a coronal hole boundary region. The nature of quasiperiodicvariability is investigated through the different temperature lines across the observedstructures. Statistically significant periods are found within the range 100-900 seconds, alongwith short period wavepackets with periods 50-100 seconds. These oscillations are discussedin terms of possible wave mechanisms. An example of a time-dependent period is observedabove the network region on the coronal hole boundary and possible theoretical origins arediscussed.Secondly, a detailed analysis is applied to an active region observed on the solar limb. Adynamic transition region loop, and closely associated ejection event are observed within theactive region. These structures are characterised by their emission line profiles; the transitionregion loop is found to have a flow geometry of -20---*40 km c 1 , and the ejection event isfound to have a velocity gradient up to -20—*50 km across its width, suggesting a rotatingtransition region structure consistent with a macrospicule.Thirdly, an upwardly propagating disturbance is observed along a coronal loop associatedwith a plage region with a velocity 50-195 km s perpendicular to the line of sight, and periodof 5 minutes. A wavelet analysis reveals that the five minute period is present in co-spatial,co-temporal chromospheric and transition region observations. This is interpreted as the first observation of a 5-mm p-mode propagating through the chromosphere, transition region andinto a coronal loop.Fourthly, an observing campaign is designed and executed to probe the connectivity betweenthe chromosphere, transition region and corona within active regions. Oscillations withinthe 3-min band are observed above the umbra of a sunspot active region. These oscillationsshow two closely separated frequencies of 6.1 & 7.1 mHz in the chromosphere, 5.9 & 7.3 mHzin the transition region and 5.9 & 7.3 mHz in the corona. These observations are interpreted asacoustic/maneto-acoustic wave modes propagating upwards through the chromosphere, transitionregion and into the corona. The frequencies are observed as oscillations in the chromosphereand transition region, and propagations in the emerging coronal loops, due to thecombined effect of the temperature scale height in the different spectral lines and the divergingmagnetic flux geometry above the sunspot. The energy flux of acoustic waves is estimated inthe different temperature lines as 28.3 erg cm 2 in the chromosphere, 201.0 erg cm2 sinthe transition region and 225.6 erg cm 2 in the corona.Finally, future work is discussed in terms of progressing the work completed, and exploitingupcoming spaced based missions." @default.
• W337054967 created "2016-06-24" @default.
• W337054967 creator A5056435681 @default.
• W337054967 date "2005-07-01" @default.
• W337054967 modified "2023-10-18" @default.
• W337054967 title "The structure and dynamic nature of the solar atmosphere" @default.
• W337054967 hasPublicationYear "2005" @default.
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