Abundance of Fe relative to H at 1.5 solar radii

Details Abundance of Fe relative to H at 1.5 solar radii Abundance of Fe relative to H at 1.5 solar radii

Jun 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975soph...42..487n&link_type=abstract

Solar Physics, vol. 42, June 1975, p. 487-496.

Astronomy and Astrophysics

Astronomy

5

Abundance, Hydrogen Atoms, Iron, Resonance Scattering, Solar Corona, Brightness, Electron Density (Concentration), Electron Scattering, Emission Spectra, Measure And Integration, Oso-7, Photoabsorption, Photosphere, Spaceborne Astronomy, Spectroheliographs

Scientific paper

The abundance of Fe relative to H is obtained by using resonantly scattered intensities of lambda 284 of Fe XV that were measured with OSO-7 and resonantly scattered intensities of L-alpha of H I that were obtained by Gabriel (1971). Because of possible differences in electron densities along lines of sight for these non-simultaneous measurements and in relative calibrations, results are rather uncertain but still indicate that the average Fe abundance relative to H in the corona appears to be at least as large as a recent photospheric abundance. Some limitations in using this method for obtaining abundances are examined for future experiments with simultaneous measurements and well calibrated detectors.

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