Wassereintrittsgeschwindigkeit zum Brunnenfilter in bezug auf die Berechnung der Filterdurchmesser

Ohne Zusammenfassung     

Grundzüge der Geotektonischen Entwicklung Südafrikas

Zusammenfassung Der südafrikanische Subkontinent kann genetisch in drei Einheiten verschiedenen Alters und unterschiedlicher Entwicklung gegliedert werden. Der älteste Teil wurde etwa vor 3000×10⁶ Jahren stabiler Schelf. Die folgende Geosynklinalbildung — nicht so eindeutig umrissen wie die erste — erlebte ihre Hauptdeformation etwa eine Milliarde Jahre später. Der jüngste Deformationsgürtel erstreckt sich parallel zum Atlantischen Ozean und dürfte ans Ende des Präkambriums zu stellen sein.Präkambrische Geosynklinalen scheinen ausgedehnter und langsamer in ihrer Entwicklung gewesen zu sein als jüngere analoge Einheiten. Früharchaische, kaum deformierte und nur schwachmetamorphe Einheiten werden aus dem östlichen Südafrika beschrieben.

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According to the structural evolution of South Africa the subcontinent can be divided into three major units of different age and historical development. The oldest part became a stable shelf about 3000×10⁶ years ago. The following geosyncline, not as well defined as the first unit, was subjected to its major folding about 1000×10⁶ years later. The youngest belt, parallel to the Atlantic Ocean, is of late Pre-Cambrian age.Pre-Cambrian geosynclines apparently have not only been considerably larger, but also required much longer time for the completion of one geotectonic cycle than during younger, post-Cambrian periods of the earth's history. The existence of hardly folded and very slightly metamorphosed early Archean rocks is described of the eastern part of South Africa.

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Résumé Conformément à l'évolution structurale de l'Afrique du Sud, cette partie du continent peut être divisée en trois unités principales d'âges et de développement historique différents. La partie la plus ancienne devint un massif stable il y a quelque 3.000×10⁶ années. Le géosynclinal suivant, qui n'était pas aussi bien défini que le premier, a subi son plissement principal quelque 1000×10⁶ années plus tard. Le segment le plus jeune, parallèle à l'Océan atlantique, est d'âge précambrien récent.Les géosynclinaux précambriens non seulement semblent avoir été considérablement plus vastes, mais ont pris également pour accomplir un cycle géotectonique un temps plus long que lors des périodes plus récentes de l'histoire de la terre, postérieures au Cambrien. L'existence de roches archéennes anciennes à peine plissées et très faiblement métamorphosées est décrite dans la partie orientale de l'Afrique méridionale.

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Messung des Ultrarot-Pleochroismus von Mineralen. XI. Der pleochroismus der OH-Streckfrequenz in Rutil,Anatas, Brookit und Cassiterit

Zusammenfassung Rutile, Cassiterite und Brookite verschiedener Fundorte enthalten entsprechend einer scharfen Absorptionslinie bei =3 kleine Mengen von Hydroxyl-Gruppen. Die Zuordnung der Absorptionslinie zur OH-Streckschwingung wurde für diese drei Minerale durch die Linienverschiebung bewiesen, die man nach hydrothermaler Deuterierung beobachtet. Die ungefähre Orientierung der OH-Gruppen konnte aus dem Pleochroismus orientierter Kristallplatten abgeleitet werden, wobei polarisierte UR-Strahlung verwendet wurde. Es wird die strukturelle Deutung gebracht. Anatas alpiner Herkunft enthält keine oder nur sehr wenige OH-Gruppen.

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Measurement of the infrared-pleochroism in Minerals. XI. The Pleochroism of the OH-stretching frequency in rutile, anatase, brookite, and cassiterite

Summary Rutile, cassiterite, and brookite from several localities contain small amounts of hydroxyl groups, based on the presence of a sharp absorption line at =3. The attribution of the absorption line to the OH-stretching vibration is proved for the three minerals by the line shift which is caused by hydrothermal deuteration. The approximate orientation of the OH-groups could be derived from the pleochroism as observed in oriented crystal plates with polarized IR-radiation. The structural interpretations are given. Anatase, however, from Alpine fissures contains no or undedectable amounts of OH-groups.

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Messung des Ultrarot-Pleochroismus von Mineralen VIII. Der Pleochroismus der OH-Streckfrequenz in Andalusit

Zusammenfassung Mikroskopisch Einschluß-freie Andalusite aus Brasilien zeigen im UR-Absorptionsspektrum ein Doppelmaximum bei zirka 2,9 und ein deutlich schwächeres einfaches Maximum bei 3,04 , die OH-Valenzschwingungen zugeordnet werden. Diese Maxima verschwinden nach mehrtägigem Glühen bei 1000° C. In Platten parallel (110) zeigt das Doppelmaximum bei zirka 2,9 einen extrem starken Pleochroismus, wobei die Bande praktisch völlig verschwindet, wenn der elektrische Vektor parallel [001] schwingt. Damit müssen zumindest die OH-Gruppen, die für diese Bande verantwortlich sind, in die Struktur eingebaut sein. Für beide Arten von OH-Gruppen werden die plausiblen Anordnungen diskutiert.

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Measurement of the infrared-pleochroism in minerals. VIII. The pleochroism of the OH-stretching frequency in andalusite

Summary Inclusion-free andalusites from Brazil show in the IR absorption spectrum a double maximum at ca. 2.9 and a much weaker single maximum at 3.04 which are interpreted as belonging to OH-stretching frequencies. The maxima disappear after annealing the specimen at 1000°C for several days. Plates parallel to (110) show a very strong pleochroism for the 2.9 -band, the peak being practically of zero height if the electric vector vibrates parallel [001]. This proves that at least the OH-groups which are responsible for this absorption band are constituents of the crystal structure. For both kinds of OH-groups the probable distributions are discussed.

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Acoustic echo-sounding techniques and their application to gravity-wave,turbulence, and stability studies

This paper is a brief summary of recent experimental studies conducted by the WPL staff in order to: (a) compare acoustic echo strengths with those predicted from measured turbulence intensities and scatter theory; (b) develop optimum experimental geometries for Doppler work, and (c) use the acoustic echo-sounder as a quantitative tool in studies of gravity wave dynamics in, and immediately above, the stable planetary boundary layer. We find that the observed acoustic echo strengths are roughly an order of magnitude greater than those predicted theoretically. This discrepancy might be in part due to partial reflection although the comparison is somewhat clouded by uncertainties in our knowledge of the equipment characteristics, propagation losses, etc. Comparisons between Doppler and in situ wind measurements give confidence in the Doppler results, but further experimentation and comparisons are needed. Preliminary use of acoustic Doppler data in a case study of gravity-wave dynamics in the planetary boundary layer has yielded boundary-layer wind speed and direction profiles which give insight into the mechanisms responsible for the wave generation. The Doppler data yield estimates of the wave associated momentum fluxes (a few dyn cm^–2) as well. The results derived from the acoustic techniques are quite encouraging, but thus far remain unsubstantiated by independent wind and flux measurements.     

Two classes of volcanic plumes on Io

Comparison of Voyager 1 and Voyager 2 images of the south polar region of Io has revealed that a major volcanic eruption occured there during the period between the two spacecraft encounters. An annular deposit ～1400 km in diameter formed around the Aten Patera caldera (311°W, 48°S), the floor of which changed from orange to red-black. The characteristics of this eruption are remarkably similar to those described earlier for an eruption centered on Surt caldera (338°W, 45°N) that occured during the same period, also at high latitude, but in the north. Both volcanic centers were evidently inactive during the Voyager 1 and 2 encounters but were active sometime between the two. The geometric and colorimetric characteristics, as well as scale of the two annular deposits, are virtually identical; both resemble the surface features formed by the eruption of Pele (255°W, 18°S). These three very large plume eruptions suggest a class of eruption distinct from that of six smaller plumes observed to be continously active by both Voyagers 1 and 2. The smaller plumes, of which Prometheus is the type example, are longer-lived, deposit bright, whitish material, erupt at velocities of ～0.5 km sec^?1, and are concentrated at low latitudes in an equatorial belt around the satellite. The very large Pele-type plumes, on the other hand, are relatively short-lived, deposit darker red materials, erupt at ～1.0 km sec^?1, and (rather than restricted to a latitudinal band) are restricted in longitude from 240° to 360°W. Both direct thermal infrared temperature measurements and the implied color temperatures for quenched liquid sulfur suggest that hot spot temperatures of ～650°K are associated with the large plumes and temperatures <400°K with the small plumes. The typical eruption duration of the small plumes is at least several years; that of the large plumes appears to be of the order of days to weeks. The two classes therefore differ by more than two orders of magnitude in duration of eruption. Based on uv, visible, and infrared spectra, the small plumes seem to contain and deposit SO₂ in their annuli whereas the large plumes apparently do not. Two other plumes that occur at either end of the linear feature Loki may be intermediate or hybrid between the two classes, exhibiting attributes of both. Additionally, Loki occurs in the area of overlap in the regional distributions of the two plume classes. Two distinct volcanic systems involving different volatiles may be responsible for the two classes. We propose that the discrete temperatures associated with the two classes are a direct reflection of sulfur's peculiar variation in viscosity with temperature. Over two temperature ranges (～400 to 430°K and >650°K), sulfur is a low-viscosity fluid (orange and black, respectively); at other temperatures it is either solid or has a high viscosity. As a result, there will be two zones in Io's crust in which liquid sulfur will flow freely: a shallow zone of orange sulfur and a deeper zone of black sulfur. A low-temperature system driven by SO₂ heated to 400 to 400°K by the orange sulfur zone seems the best model for the small plumes; a system driven by sulfur heated to >650°K by hot or even molten silicates in the black sulfur zone seems the best explanation for the large plume class. The large Pele-type plumes are apparently concentrated in a region of the satellite in which a thinner sulfur-rich crust overlies the tidally heated silicate lithosphere, so the black sulfur zone may be fairly shallow in this region. The Prometheus-type plumes are possibly confined to the equatorial belt by some process that concentrates SO₂ fluid in the equatorial crust.