C IV fluxes from the Sun as a star, and the correlation with magnetic flux

Details C IV fluxes from the Sun as a star, and the correlation with magnetic flux C IV fluxes from the Sun as a star, and the correlation with magnetic flux

Aug 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988jila.reptr....s&link_type=abstract

Final Report Joint Inst. for Lab. Astrophysics, Boulder, CO.

Astronomy and Astrophysics

Astrophysics

Chromosphere, Distribution Functions, Magnetic Flux, Solar Flares, Spatial Resolution, Optical Thickness, Solar Maximum Mission, Spectroheliographs, X Ray Spectra

Scientific paper

A total of 144 C IV wavelength 1548 Solar Maximum Mission (SMM)-UVSP spectroheliograms of solar plages were analyzed, some of which are series of exposures of the same region on the same day. Also analyzed were the C IV wavelength 1551 rasters of plages and C IV wavelength 1548 rasters of the quiet sun. The sample contained data on 17 different plages, observed on 50 different days. The center-to-limb variations of the active regions show that the optical thickness effects in the C IV wavelength 1548 line can be neglected in the conversion from intensity to flux density. As expected for the nearly optically thin situation, the C IV wavelength 1548 line is twice as bright as the C IV 1551 line. The average C IV wavelength 1548 flux density for a quiet region is 2700 ergs/cm/s and, with surprisingly little scatter, 18,000 erg/cm/s for plages. The intensity histograms of rasters obtained at disk center can be separated into characteristic plage and quiet sun contributions with variable relative filling factors. The relationship between the C IV and magnetic flux densities for spatially resolved data is inferred to be almost the same, with only an additional factor of order unity in the constant of proportionality.

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