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

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

Author
Saar, S. H.
Published
Aug 30, 1988.
Physical Description
1 electronic document
Additional Creators
Brown, A., Bennett, J., Schrijver, C. J., and Linsky, J. L.
Online Version

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Unclassified, Unlimited, Publicly available.
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Summary
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.
Other Subject(s)
Collection
NASA Technical Reports Server (NTRS) Collection.
Note
Document ID: 19890004016.
Accession ID: 89N13387.
NAS 1.26:182719.
NASA-CR-182719.
Terms of Use and Reproduction
No Copyright.
View MARC record | catkey: 15693015