Quiet and active solar emission of Fe XV 284 A radiation

Details Quiet and active solar emission of Fe XV 284 A radiation Quiet and active solar emission of Fe XV 284 A radiation

Jul 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975mnras.172..159a&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 172, July 1975, p. 159-173.

Astronomy and Astrophysics

Astronomy

14

Far Ultraviolet Radiation, Iron, Solar Corona, Solar Radiation, Spaceborne Astronomy, Spectroheliographs, Line Spectra, Oso-7, Radiant Flux Density, Solar Activity Effects, Sunspots

Scientific paper

Daily intensity contours of Fe XV line emission at 284 A obtained from OSO-7 EUV spectroheliograph observations are analyzed to separate quiet-sun and active-region emissions during the period from May 1972 to March 1974. Measurements were made of the central, equatorial limb, and polar intensities as well as the quiet-sun (Q), active-region (AR), and total fluxes. The Q and AR fluxes are found to vary almost proportionally with sunspot number, and the Q intensity is shown to fit an exponential emission model with a scale height of 0.125 solar radii. Fluxes from separate active regions are found to be closely related to plage fluxes, and the relation is shown not to change over plage lifetimes. The absolute emission from the quiet corona is compared with expected values based on eclipse electron densities, and the coronal irregularity factor is estimated. This factor is shown to vary from 4 near the surface to 30 at 1.5 solar radii. Coronal densities within well-developed active regions are found to be about five times greater than the quiet-sun value.

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