Abstract1-(4-Methylsulfonyl)-2-thione-4-aryl-5-Z-6-methyl and oxyalkyl-imidazoles were synthesized from different tetrahydropyrimidinethiones and aryl sulfonyl chloride. These compunds were tested for metal chelating effects and to determine the phrase in which inhibition occured between two physiologically pertinent compunds and carbonic anhydrase (CA) isozymes I and II (hCA I and II), butyrylcholinesterase (BChE) and acetylcholinesterase (AChE). AChE was detected in high concentrations in the brain and red blood cells. BChE is another enzymes that is abundant available in the liver and released into the blood in a soluble form. Newly synthesized hetaryl sulfonamides exhibited impressive inhibition profiles with Ki values in the range of 1.42–6.58 nM against hCA I, 1.72–7.41 nM against hCA II, 0.20–1.14 nM against AChE and 1.55–5.92 nM against BChE. Moreover, acetazolamide showed Ki values of 43.69 ± 6.44 nM against hCA I and 31.67 ± 8.39 nM against hCA II. Additionally, tacrine showed Ki values of 25.75 ± 3.39 nM and 37.82 ± 2.08 against AChE and BChE, respectively.

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Almost all observations of the sun, including all kinds of spectropliotometry, magnetic field and radial velocity measurements, and also spectroheliographic researches supply us with only two-dimensional (flat) information about the object. We obtain data on the distribution of a physical parameter in two-space dimensions (in some cases one of these dimensions is the wavelength in the spectrum) or in space-time dimensions. Only when we take a cinema-film (MAMEDOV, 1966) of the spectral changes over the disk with a slowly moving image of the sun on the slit, we have a real possibility of obtaining three-dimensional information: two space dimensions Fig. la. Fig. lb.and one wavelength dimension. This seems to be true only if the time scale of the physical processes under investigation is greater than the cinema exposure time. Thus we have spectrograms taken so near to one another on the object that they form a continuous sequence of spectral changes over the object (a portion of the solar disk, sunspots, flares, chromosphere). The method was previously described by Mamedov and applied to the H and K lines. In some respects it is similar to the well-known method of Deslandres, although the latter was restricted to the case of two-dimensional information on the radial velocity distribution over the solar disk.The same method has now been applied to the chromospheric Ha line. The band Solar Physics 6 (1969) 41-43; O D. Reidel Publishing Conzpany, Dordrechf -Holland