In this paper I briefly review the history of the formation of first elements, the first molecules and the first stars. The exact path of formation of the first molecules is explained in some detail. The role of molecules in the formation of the first stars is emphasized. Finally the principles of the calculation and the measurement of the process of hydrogen molecule formation in the collision of negative hydrogen ions with hydrogen atoms is briefly explained., Martin Čížek., and Obsahuje seznam literatury
Two monogenean species are recorded from a blotched fantail ray, Taeniurops meyeni (Müller et Henle) (Dasyatidae), kept in a public aquarium at the Guangzhou Ocean World. Heterocotyle taeniuropi sp. n. was obtained from the gills. It is similar to Heterocotyle similis Neifar, Euzet et Ben Hassine, 1998 and H. scotti Neifar, Euzet et Ben Hassine, 1998, both of which have a similar male copulatory organ, but it can be distinguished from these two species by aspects of the morphology of the male copulatory organ, which is tubular, straight or slightly curved with a sclerotized accessory piece and an asymmetrical funnel-shaped opening at the proximal end, and recurved at the distal end. Dendromonocotyle pipinna Chisholm et Whittington, 2002, which is a new record for Chinese waters, was collected from the body surface of the same host. Its main features are almost the same as in the original description, except that it exhibits a variable number of marginal papillae.
An infection with Septata intestinalis was diagnosed in a 35-year-old AIDS patient without diarrhoea. The diagnosis was based on morphological examinations of a duodenal biopsy specimen. Serum antibodies were detected reacting with spores of Encephalitozoon cuniculi. Spores of S. intestinalis and E. cuniculi stained with Brown Hopps Gram stain showed a red colour (Gram negative) and not a blue/black colour which was described for microsporidian spores in tissue.
Various instruments were used to observe the solar corona and prominences near or at the time of solar eclipse, 22 July 1990. The white-light solar corona pictures were observed nearly up to R = 3 (solar radii) with the Úpice Observatory eclipse team at Markovo. Both emission line intensities (the green and red corona) and prominences were obtained at Lomnický Peak coronal station. These data sets are used to identify active coronal regions. A large coronal hole was observed above the south pole and extending nearly up to R = 2.5. Large-scale structure of the white-light corona is very complicated. There are many streamers nearly equally distributed around the whole Sun (except the south pole). Several streamers above the solar surface are not extended radially with
their height. In the NE quadrant 4 voids are clearly seen at the height of about R = 2. A slight excess of the white light corona is in favor of the west limb, however, the emission corona has an opposite meaning. Green and red corona, similarly as prominences, showed rapid changes in active regions over the eclipse period, however, any CME was not directly observed. The integral brightness of the 22 July 1990 white-light corona was estimated as JK = 1.32 x 10~6 and the ellipticity, a + b = 0.04. The white-light corona was nearly a maximum type.