L'or dans la métallogenie du massif de Bohême

Les minéralisations aurifères du massif de Bohême sont représentées par plusieurs types morphologiques et paragénétiques, dont l'origine est expliquée par trois modèles genétiques: I — un modèle volcanogénique pour les minéralisations sulfurés stratiformes, II — un modèle hydrothermal-métamorphique pour les minéralisations de quartz aurifères synmétamorphiques, de morphologie très variable et caractérisées par la présence de minéraux de Bi, Te, Mo et W (scheelite), III — un modèle hydrothermal de shear zones aurifères, pour les minéralisations postmétamorphiques, caractérisées par des teneurs en argent plus élevées (electrum) ou par une minéralisation complexe à stibine et or.Les complexes volcanosédimentaires, principalement protérozoiques, sont considérés comme les sources de l'or pour les minéralisations plus tardives, liées à la cratonisation du massif de Bohême. Au course de l'évolution géotectonique et métallogenique du massif de Bohême les conditions de mis en place des minéralisations aurifères ont évolué d'un contrôle initialement lithologique vers un contrôle lithologique et structural pour aboutir à un contrôle exclusivement structural. Ce développement a été accompagné par une augmentation de la taille des particules d'or et par leur pépitisation dans les minéralisations tradives.     

Real-time simulation of a potential magnetic field in a post-flare arch

We analyze the X-ray observations on 7–8 November of the last revival of a giant coronal arch first observed in the morning hours of 6 November, 1980. We compare these data with observations of earlier revivals of this arch, in order to determine whether the successive brightenings repeat without any apparent modification, or whether they show a varying behavior as they keep occurring. We also examine the magnetic structure of the revived arches in order to ascertain whether the subsequent phenomena involve the same magnetic configuration. The information about the magnetic structure of the last revival is the best we have, because the revival started close to the time of the Kitt Peak magnetogram which has been used for the magnetic modelling of the whole series of these giant arches.We conclude that while there seems to be some plasma depletion in the 7–8 November event, the real-time magnetic field modelling on this date seems to fit the observed footpoints better than the modelling on 6 November which had to use the same magnetogram for a situation occurring 24 to 36 hours earlier. The general topology does not show any significant change, apart perhaps in the field line inclination, but some flux tubes seem to have disappeared between 6 and 7 November. Nevertheless, both X-ray and H observations indicate that this magnetic structure basically kept its identity for more than 4 days.We also compare the two existing interpretations of the arch revivals: re-excitation of a permanent pre-existing structure (after Hick and vestka, 1987) and formation of each brightening through a separate reconnection (after Poletto and Kopp, 1988). Unfortunately, proximity to the limb does not allow one to decide between these two alternatives; it is suggested to look for other series of arch revivals utilizing our present knowledge about the behavior of the chromospheric footpoints of giant arches.     

The dynamical flattenings of Mercury and Venus

The method which is used to calculate the dynamical flattenings % MathType!MTEF!2!1!+-% feaafeart1ev1aaatCvAUfeBSjuyZL2yd9gzLbvyNv2CaerbuLwBLn% hiov2DGi1BTfMBaeXafv3ySLgzGmvETj2BSbqefm0B1jxALjhiov2D% aebbfv3ySLgzGueE0jxyaibaiiYdd9qrFfea0dXdf9vqai-hEir8Ve% ea0de9qq-hbrpepeea0db9q8as0-LqLs-Jirpepeea0-as0Fb9pgea% 0lrP0xe9Fve9Fve9qapdbaqaaeGacaGaaiaabeqaamaabaabcaGcba% Gaamisaiabg2da9iaacIcacaWGdbGaeyOeI0YaaSaaaeaacaaIXaaa% baGaaGOmaaaacaGGOaGaamyqaiabgUcaRiaadkeacaGGPaGaaiykai% aac+cacaWGdbaaaa!4717!\[H = (C - \frac{1}{2}(A + B))/C\] of the Earth and Moon meets with difficulties when it applies to Mercury and Venus. In this paper, after the calculation of the dimensionless moment of inertiaC/MR ² by solving the Emden equation, the effectiveness of the method deriving dynamical flattening from the observed value of the Mercury's obliquity is analysed based on the resonance rotation theory. Some suggestions are made for the future space explorations. Finally, the ranges of dynamical flattening and of the obliquity of Venus are calculated.     

Solar and interplanetary observations of the mass ejection on 7 May, 1979

We present observations of a mass ejection that was observed by five different instruments along its way from the solar surface to more than 100 solar radii. The instruments involved are the ground-based H coronagraph at Wrocaw, the white-light SOLWIND coronagraph on board the P78-1 satellite, zodiacal light photometers of the HELIOS B spacecraft, in situ plasma detectors and magnetometers on board the HELIOS B spacecraft, and interplanetary scintillation measurements on the ground. By using a CAT-scan analysis of the images obtained by the SOLWIND coronagraph near the Earth and HELIOS B photometers placed at 0.3 AU perpendicular to the Earth-Sun line, we have been able to get a three-dimensional density reconstruction of the mass ejection and fit the best velocity curve for its propagation. Although problems exist in smoothly joining the height-time curves (for instance, we had to reduce the brightness of the SOLWIND data by more than a factor of two to make the data sets agree photometrically), both this analysis and direct measurements by the other experiments clearly indicate higher speeds at greater distances from the Sun. The plasma acceleration in this case was obviously not limited only to distances within 3 R ₀ , as is usually the case, but continued beyond the outer limit of the coronagraph view at 8 R ₀ .The National Center for Atmospheric Research is sponsored by the National Science Foundation.     

Dynamical evolution of the rotation of Venus

By considering the torque of the bodily tides, the effect of the core-mantle viscous coupling and the torque of the atmospheric tides have been obtained by numerical calculation: the evolution of the spin angular velocity and the obliquity of the Venus are calculated numerically with the step-variable Runge-Kutta method of 7th order; and 7 sets of the probable Cytherean spin evolution have been obtained. It is indicated that the present spin state of Venus is the result of long-term evolution within the reasonable ranges of some disposable parameters. The early spin period is between 7 h to 2 d and the corresponding obliquity is about 90 ° ~ 100 °. The effects of the torques of body and atmospheric tides and the core-mantle viscous coupling of Venus on its spin angular velocity could nearly cancel out each other about a billion years ago. Therefore, Venus could have been captured in a spin-orbit resonant state by the gravitational torque of the Earth on the permanent deformation part of Venus; and this resonant state has lasted up to the present time.     

Modeling of air stripping from volatile organic compounds in biological treatment processes

The removal of volatile organic compounds from biological treatment processes occurs through several mechanisms. These include biodegradation, adsorption onto solids, and air stripping or volatilization to the atmosphere. Volatilization results in fugitive emissions to the atmosphere, which is largely uncontrolled. Recent regulations have called for increased evaluation and control of inadvertent volatile organic compounds emissions from treatment processes. The use oxygen as a parallel volatile compound is extremely useful for prediction of volatile organic compounds removal by air stripping. In this study, the simultaneous biodegradation and air stripping of volatile organic compounds, based on steady state mass balance are examined and a general approach to estimating the dominant removal mechanism is developed. A Monte Carlo simulation technique was used to estimate air stripping over a wide range of operating conditions. Several volatile organic compounds were selected for this study. The results showed the values drived from the model correspond with the experimental data for benzene, toluene, methylene chloride, trichloroethylene, and methyl isobutyl ketone.     

Bryozoan event from Middle Miocene (Early Badenian) lower neritic sediments from the locality Kralice nad Oslavou (Central Paratethys,Moravian part of the Carpathian Foredeep)

Fossil Bryozoa occurs usually in shallow-water environments. One of the rare deep-water associations of Bryozoa has been studied in a profile at Kralice nad Oslavou. According to studies of foraminifera, the paleodepth was more than 150 m and less than 500 m. The bryozoan assemblages are poor, consisting of four species only, dominated by Tervia irregularis (Cyclostomatida) and Reteporella kralicensis sp.n. (Cheilostomatida), a new species being described in detail.     

Salt tectonics in pull-apart basins with application to the Dead Sea Basin

The Dead Sea Basin displays a broad range of salt-related structures that developed in a sinistral strike-slip tectonic environment: en échelon salt ridges, large salt diapirs, transverse oblique normal faults, salt walls and rollovers. Laboratory experiments are used to investigate the mechanics of salt tectonics in pull-apart systems. The results show that in an elongated pull-apart basin the basin fill, although decoupled from the underlying basement by a salt layer, remains frictionally coupled to the boundary. The basin fill, therefore, undergoes a strike-slip shear couple that simultaneously generates en échelon fold trains and oblique normal faults, trending mutually perpendicular. According to the orientation of basin boundaries, sedimentary cover deformation can be dominantly contractional or extensional, at the extremities of pull-apart basins forming either folds and thrusts or normal faults, respectively. These guidelines, applied to the analysis of the Dead Sea Basin, show that the various salt-related structures form a coherent set in the frame of a sinistral strike-slip shearing deformation of the sedimentary basin fill.