Spectroscopic differences between solar-type cluster stars and the sun

Details Spectroscopic differences between solar-type cluster stars and the sun Spectroscopic differences between solar-type cluster stars and the sun

Feb 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...219..942b&link_type=abstract

Astrophysical Journal, Part 1, vol. 219, Feb. 1, 1978, p. 942-946.

Astronomy and Astrophysics

Astrophysics

9

Abundance, Astronomical Spectroscopy, Dwarf Stars, F Stars, G Stars, Late Stars, Solar Spectra, Star Clusters, Coma, Cyanogen, Molecular Spectra, Spectral Resolution

Scientific paper

Two-angstrom-resolution spectrograms reveal the strength of 3871 A (CN) relative to 3859 A (Fe I) and 3883 A (CN) relative to 3878 A (Fe I) to be systematically greater in late F and G dwarfs in the Hyades cluster than in the Coma cluster. This difference is explained as a normal consequence of the general enrichment of the metals in the Hyades and the dependence of the CN abundance on the product of the C and N abundances. The 3859/3871 and 3878/3883 ratios in the spectrum of the Ursa Major Cluster dwarf HD 115043 indicate that its surface gravity and metallicity are similar to members of the Coma cluster. The simplest interpretation of the sun's spectrum is that its surface gravity and metallicity are similar to those of members of the Hyades cluster.

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