Optical and EUV Observations of the Solar Atmosphere

Details Optical and EUV Observations of the Solar Atmosphere Optical and EUV Observations of the Solar Atmosphere

Mar 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000phdt.........2g&link_type=abstract

Ph.D. Thesis, The Queen's University of Belfast, Belfast, N. Ireland.

Computer Science

1

Euv, Sun, Corona, Transition Region, Eclipse, Secis, Blinker, Network, Solar Wind

Scientific paper

This thesis presents the results of optical and EUV observations of the solar atmosphere ranging in height from the photosphere to the corona. In the first sections, the morphology and dynamics of the photosphere, chromosphere, transition region and corona are studied with the Coronal Diagnostic Spectrometer (CDS) and the Michelson Doppler Imager (MDI) onboard the Solar and Heliospheric Observatory (SOHO). These results are compared to, and found to be consistent with, current solar atmospheric models. We also use the density sensitive Si IX (349.9 A/341.9 A) and Si X (356.0 A/347.7 A) line ratios, observed with CDS, to study the radial and angular variation of electron density in the corona. These observations are found to agree extremely well with recent magnetohydrodynamical models of the corona and solar wind. The design and testing of the Solar Eclipse Coronal Imaging System (SECIS) is also described in the final section. This instrument was designed to search for short-period modulations in the Fe XIV (5303 A) solar corona seen either during a total eclipse or with a coronagraph. Initial results from SECIS observing programs at the John W. Evans Solar Facility coronagraph in New Mexico, and from the 1999 August 11 total solar eclipse are also discussed.

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