Profiles and Wavelength of Spectrum Lines in the Solar Chromosphere

Citation

Parker, James Mervin (1954) Profiles and Wavelength of Spectrum Lines in the Solar Chromosphere. Dissertation (Ph.D.), California Institute of Technology. doi:10.7907/GC46-VM62. https://resolver.caltech.edu/CaltechETD:etd-01122004-160233

Abstract

NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document. Observations have been made of the spectrum of the solar chromosphere outside of eclipse. The spectral region covered extends from [...] to [...] and from [...] to [...]. In addition, The O I triplet at [...] was photographed. In all, 1882 emission lines were photographed, and measured for wavelengths. Photographic intensity profiles were found for 530 of the lines, through the use of a microdensitometer. 330 of these lines were due to the Swan hands of C2. These lines were measured for total intensity, and a rotational temperature of 4600[degrees]K derived. The other 200 lines were reduced using the method of Voigt profiles. The width of the lines as a function of atomic weight was examined in the light of several assumptions, and it was found that the best interpretation was that of low temperature, of the order of 5000[degrees]K to 6000[degrees]K and an overlying turbulent motion which varies with height in the chromosphere. The interpretation of the line contours on this basis was performed using the model chromosphere due to van de Hulst.

Thesis Files