The Chemical Composition and Ultra-Violet Excess of G Dwarfs

New values of [Fe/H] have been derived for 18 of the G dwarfs for which Wallerstein has published determinations of abundance; the original measurements of equivalent width have been subjected to different methods of analysis. The general agreement with the earlier results of Wallerstein and his collaborators is good; however, the present values of [Fe/H] of + 0.2 or + 0.3 obtained for the Hyades differ considerably from those derived previously. It appears that for most G dwarfs in the solar neighbourhood the ultra-violet excess does not depend to any large extent on factors other than metal abundance, surface gravity and temperature. The question of the metal abundance of the Sun relative to that of other stars will be considered in more detail in a later paper.