Oocyst morphology and endogenous developmental stages are described for Choleoeimeria salaselensis sp. n. from the gall bladder of 10 horned vipers, Cerastes gasperettii Leviton and Anderson, in Saudi Arabia. Sporulated oocysts are ellipsoidal, 23 × 15 (22-25 × 14-17) µm, length/width ratio (L/W) 1.5 (1.4-1.6), each with 4 sporocysts (Eimeria-like), but lack a micropyle, polar granules and oocysts residuum. Sporocysts are ellipsoidal, 8 × 5 (7-9 × 5-6) µm, L/W 1.5 (1.4-1.6), and Stieda, substieda and parasubstieda bodies are all absent, but a longitudinal suture, which divided the sporocysts into 2 plates, is present. Endogenous development is confined to epithelial cells in the bile duct and gall bladder; mature meronts were 11 × 7 µm, each with 10-16 merozoites, microgamonts were ~12 µm wide, and macrogamonts were ~16 µm wide with a prominent nucleus and wall-forming bodies. Given these two diagnostic features, sporocysts with a suture and composed of two plates and endogenous development limited to the biliary epithelium, we believe this coccidium is best classified as a member of Choleoeimeria Paperna et Landsberg, 1989. There are 5 known Eimeria species from vipers that have sporocysts somewhat similar in size to those of our new form, but all of them have much larger oocysts and larger sporocysts, some of which differ significantly in shape; there are not yet any Choleoeimeria species known from the Viperidae.
Time and latitude observations, made by the circumzenithal at the Geodetical Observatory Pecný (Ondřejov) in the years 1970-1983, were analysed and some secular and periodical terms were proved. These results are studied from the standpoint of possibilities of their geodynamical interpretation: determination of the secular variation of the station position, detection of the secular, Chandler's and annual polar motion from optical measurements at the single station, and tidal influence on the variation of the local plumb-line.
High resolution UV spectroscopic observations of the binary symbiotic star AG Peg obtained with the IUE satellite in the periode 1978-81 are analyzed. The variability of the fluxes and the radial velocities of emission lines accordingto orbital phase are presented, The observaions support a binary model with mass transfer from a hot rotationaly unstable subdvarf to a cool M giant.