Abundances of 11 elements are determined in the atmosphere of the manganese star HR562 = HD11905 (B8III, Te = 14000 K, log g=3.5). The deficit of iron of 0.9 dex is extreme among HgMn stars. The excess of mercury abundance amounts to 4.8 dex.

Photometric and spectroscopic variability of HR 6127 was found. The value of the magnetic axis inclination was derived from the radial velocity variations of metallic lines. The star was classified as cool CP2 star.

The Survey of principal physical characteristics of the atmospheres of Am stars has been carried out. The anomalies of chemical composition have been discussed. The deficiency in C, O, Mg, Ca, and Sc alongside the excesses of heavier-than-Ni elements, with respect to Fe has been pointed out. The hypothesis on the nature of the observed anomalies are briefly discussed.

High-resolution observations of the doublet LiI-6707 A were made to study the abundance of lithium in a sample of Am, δDel, and reference stars. It is found that Am and δDel stars may be underabundant, normal or overabundant in lithium (normal Li abundance meaning log NLi = 3.0 with log NH = 12).

Preliminary results are presented on the behaviour of the feature at 6708 Å; the location of the observed feature coincides with the doublet of Li I 6707.761 and 6707.912 Å.

Prelimary results from an optical region study of the metallic-lined star 32 Aquarii indicate Teff = 7600 K, log g = 3.10, ξ = 4.6 km s−1, and an iron abundance about one-half solar.

The observations of AmFm, λ Booti, HgMn and He rich stars that are explained without any arbitrary parameter by diffusion are briefly reviewed, followed by those observations that are not explained by this simple model. Mass loss is then shown to explain a large fraction of the observations that are not explained in the parameter free model. It seems to play a role in the λ Booti, AmFm, He rich and the hot horizontal branch stars. It is only of about 10−15 to 10−13 Mo/yr. Abundance anomalies then help to determine stellar hydrodynamics. It is finally suggested that recent observations of Li underabundances in F stars of the Hyades represent an extension of the AmFm star phenomenon.

A possibility is analyzed of explaining the chemical anomalies of chemically peculiar (CP) F-A-B stars basing on the assumption of the formation of a large number of moonlike planetoids both in the course of separation of the components and in late stages of close binary evolution.

Primitive igneous differentiation of such planetoids results in their crust becoming deficient in Mg, Ca, Sc and enriched in Pe, Sr, Ba, and the Rare Earths. Infall of such planetoids or crust fragments ejected in their collisions with one another onto an A star makes it Am-type. The deficiency of some elements relative to normal abundance can be accounted for if one assumes that these elements present in the matter streaming from one binary component to another condense with subsequent rain-out into a component or formation of the planetoids.

The more diverse and complex anomalies (including the separation of isotopes) can be explained in the same context of the close binary evolution by invoking the ideas of magnetic cosmochemistry which considers the consequences of extremely nonequilibrium processes associated with the flow of magnetic-field generated electrical currents through a rarefied matter in space.