Lambda 5303 Fe XIV density models of the inner solar corona

Details Lambda 5303 Fe XIV density models of the inner solar corona Lambda 5303 Fe XIV density models of the inner solar corona

Mar 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978soph...57..119f&link_type=abstract

Solar Physics, vol. 57, Mar. 1978, p. 119-128.

Physics

2

Atmospheric Models, Electron Density Profiles, Line Spectra, Solar Corona, Solar Spectra, Spectral Energy Distribution, Density Distribution, Iron, Luminous Intensity, Solar Rotation

Scientific paper

The Sacramento Peak Observatory's 40-cm coronagraph was used with an emission line photometer to observe the distribution of 5303-A Fe XIV brightness as a function of position angle, height above the limb, and time. These data were used to construct volume-emissivity models which in turn yielded estimates of electron density distribution in the lower solar corona as a function of latitude and longitude for several specific periods in 1973 and 1975. An upper limit for the inferred electron density in coronal hole regions is set at log N(e) = 7.4 for an altitude of 1.15 solar radii. Density models from late 1973 indicate an evolutionary trend toward a rather regular four-lobed appearance of coronal material; models from 1975 suggest that this characterization persisted for at least 27 solar rotations. A decrease in the total integrated Fe XIV intensity of a factor of 2.9 is inferred to have taken place between 1973 and 1975.

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