Determination of the total amount of hydrogen atoms in a quiescent prominence

Details Determination of the total amount of hydrogen atoms in a quiescent prominence Determination of the total amount of hydrogen atoms in a quiescent prominence

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984soph...93..317g&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 93, July 1984, p. 317-324.

Physics

Hydrogen Atoms, Metallicity, Solar Atmosphere, Solar Prominences, Solar Spectra, Stellar Composition, Emission Spectra, Scandium, Ultraviolet Spectra, Yttrium, Zirconium

Scientific paper

A brief quantitative review of the determination of the chemical composition of the Sun and stars is given. The method of estimation of the total amount of hydrogen atoms in a prominence is considered. The values of relative abundances of some infrequent elements in the solar atmosphere are refined using metal emission lines in the spectrum of a quiescent prominence. The most probable values of relative abundances for yttrium ≅1×10-9, zirconium ≅2×10-9, and scandium ≅3.8×10-9 are derived.

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