The solar metallicity and colors from spectral quantification

Details The solar metallicity and colors from spectral quantification The solar metallicity and colors from spectral quantification

Jun 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...222.1032b&link_type=abstract

Astrophysical Journal, Part 1, vol. 222, June 15, 1978, p. 1032-1042.

Astronomy and Astrophysics

Astrophysics

30

Metals, Solar Spectra, Stellar Spectrophotometry, Ubv Spectra, Abundance, Star Clusters

Scientific paper

The method of spectral quantification is used to determine the UBV colors of the sun. The summed strength of several Balmer lines and the B-V color for solar-type stars in the Hyades are correlated with a measure of the solar Balmer-line strength, yielding the color the sun would have if it had the Hyades blanketing. The color the sun would have for the blanketing of Coma stars is obtained from observations of such stars, and a similar procedure is employed to obtain two preliminary solar U-B colors appropriate for the Hyades and Coma blanketing, respectively. Direct measures of the strength of various metallic lines in the solar spectrum are then compared with those in the Hyades and Coma spectra to determine the proper interpolation for finding the colors appropriate for the actual solar blanketing. It is shown that all significant differences between the reported UBV colors and those available in previous literature are eliminated when the latter are corrected for the observed solar line blanketing. The results indicate that the solar spectrum, which defines spectral type G2 V, apparently has UBV colors typical of stars classified about 0.1 spectral type later.

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