Physics
Scientific paper
Jun 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998phdt........50y&link_type=abstract
Ph.D. Thesis, University of Cambridge
Physics
4
The Sun, Euv, Spectra, Corona, Transition Region, Stellar Coronae, Abundances
Scientific paper
A variety of extreme ultraviolet (EUV) spectra from satellite and rocket-borne instruments are studied and used both as a check on the quality of theoretical atomic data and to determine physical parameters for the solar atmosphere. In addition, atomic data for several ions found in the solar atmosphere are assessed for incorporation into the CHIANTI atomic database. For some of these ions it was necessary to compute data using the SSTRUCT atomic code. Data from the Skylab S082A instrument together with lines observed in the visible portion of the solar spectrum at an eclipse are used to derive estimates of the Ar/Ca relative abundance in the solar corona. A spectrum obtained by the Solar Extreme ultraviolet Rocket Telescope and Spectrograph (SERTS) is analysed thoroughly in order to check the accuracy of atomic data in the CHIANTI atomic database, and to derive electron densities for the observed region. Several data-sets obtained with the Coronal Diagnostic Spectrometer (CDS) onboard the Solar and Heliospheric Observatory (SOHO) are studied. The relative calibration of the two bandpasses of the Normal Incidence Spectrometer of CDS is investigated by comparing silicon and iron emission lines in different sets of spectra. Large variations in the Mg/Ne relative abundance are found within a single active region, and electron densities are derived. The spectra of an intense polar plume observed by CDS are analysed and physical parameters derived. Comparisons are made with the parameters for the coronal hole background. EUV spectra from the stars Alpha Centauri and Procyon obtained by the Extreme Ultra-Violet Explorer (EUVE) are presented. The physical parameters of these two solar-like stars are then compared.
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