Statistical study of Am stars in spectroscopic binary systems

Using the Am components in spectroscopic binaries, the region of metallicism in the (log m, log R) diagram is statistically discussed. The metallic-line characteristics appear in a slightly evolved stage near the Main Sequence within a belt characterized by log g = 3.8-4.2, for which the radii R/R(Sun) = 1.5-2.7. The distribution in the diagram indicates that appreciable differences should exist in the abundances as well as in the mixing lengths of the atmospheres of the Am components. Synchronism between rotation and revolution for the Am components is discussed, and it is clearly found that the synchronism holds accurately for the Am binaries with periods less than about six days, but for those with periods between six and ten days some Am components corotate and some do not, perhaps depending upon their ages. Using the Am spectroscopic binaries with periods less than twelve days, it is found that the excess of metallicity is statistically correlated with the rotational velocity; and it is confirmed that the metallicity grossly decreases with increasing rotational velocity. If the effect of a non-Am secondary component is eliminated from a [m1]-value for the combined light, the correlation between metallicity excess and rotational velocity for the Am components only should approach Δ[m1]/ΔV (km s-1) = -0.00077. (Auth.)