Anomalous propagation of refracted waves beneath the Orlík water reservoir, Czech Republic

The Orlík water reservoir was built on the Vltava River in the places where the river crosses the geological unit called the Central Bohemian Pluton. Previous geological studies have disclosed no significant lateral inhomogeneity or fault zone in the close vicinity of the reservoir. However, repeated levellings, performed there in the 1950s and 1960s, revealed a systematic subsidence of the Vltava River valley. Using these measurements, the idea of the tectonic origin of the valley was even formulated. Recent seismic observations have also attracted attention to this region. Namely, a macroseismically felt earthquake occurred there on January 13, 2007, and many weaker earthquakes have been recorded by local seismic networks since 1992. To increase the accuracy of locating these seismic events, recently we have carried out refraction measurements along a short profile across the Orlík reservoir. These authors smoothed the observed travel times and derived a 1-D velocity model of the shallow crustal structure for the Orlík region. In the present paper, using the same refraction measurements, we study some anomalies in wave propagation beneath the Orlík reservoir. In particular, it is shown that the passage of seismic waves beneath the reservoir leads to their time delays and spectral changes. Moreover, we have also recognised similar time delays in earlier data from the nearby international profile CEL09 in the places where the profile crosses the Orlík reservoir.     

Growth of complex sheeted zones during recycling of older magmatic units into younger: Sawmill Canyon area,Tuolumne batholith,Sierra Nevada,California

In Sawmill Canyon, located near the eastern margin of the Tuolumne batholith, central Sierra Nevada, California, a series of petrologically and structurally complex, magmatic sheeted zones intrude older granodioritic units (Kuna Crest and equigranular Half Dome) and in one case truncate these units along a sharp contact. These sheeted zones (a) consist of numerous batches of (now frozen) magma, (b) display clear outward growth directions, (c) were actively deforming during and after emplacement resulting in magmatic folds, faults and multiple magmatic mineral fabrics, and (d) are the location of numerous, but localized magma flow structures (schlieren-bounded tubes, troughs, megacryst-rich pipes) and instabilities (load casts, flame structures, slumps, diapirs, ridge and pillar structures). Geochemical data indicate that the sheeted zones largely consist of magmas derived from the Half Dome granodiorite with some late Cathedral Peak granodiorite pulses, and with fractionation and flow sorting forming widespread layering in the above structures.     

Optical identifications of radio sources in the 5C areas

Results from optical identifications in the areas 5C1, 5C2, and 5C3 are summarized and compared. The identification rate is the same in all three areas within the statistical and systematic accuracy. No red quasars seem to exist; there may be a possible new group of bright starlike identifications. Galaxies deviate appreciably from their radio barycenter while quasars do not.     

Zur Auswertung astronomischer Aufnahmen mit dem automatischen Flächenphotometer

By measuring astronomical plates point by point by a microdensitometer information of very high redundancy is provided together with considerable noise due to the grains of the emulsion. In order to get astronomically relevant parameters the signal has to be separated from this noise and the data should be compressed. A chain of processing steps is described and analysed the crucial part of which being a variable twodimensional filter. This filter fits automatically its own band width to the incoming signal and reduces the number of data considerably (up to a factor of about 100). It is based on a modified HAAR transform and can be implemented easily on a relatively small processor working on line with the microdensitometer. The optimal separation of the noise is accomplished by a further variable digital filter (twodimensional KALMAN filter performed on an universal computer) the band width of which is also steered by the HAAR filter. The stars and galaxies in a larger field of the plate are picked up in the domain of the HAAR transform. Finally, the astronomically relevant parameters (coordinates and brightness of stars; furthermore diameter, axial ratio, position angle, perturbation, bright core et al. for galaxies) are obtained from the expansion of the intensity distribution into potential moments. The method is applicable e.g. to the determination of the brightness or colour distribution in a single galaxy or to the photometry of all stars and galaxies in a large part of the plate. The star photometry is obtained by integrating the intensity distribution of each object, if the characteristic curve of the plate is known from a calibration wedge copied onto the plate. Then no photoelectric sequency across the whole brightness range under consideration is needed besides of the zero point of the magnitude scale.     

Evolution effects in the distribution of distant galaxies?

The amplitudes of the two-point correlation function for galaxies are compared for galaxy catalogues extending to different depths. Strong evolution effects in the pattern of galaxy distribution seem to be present suggesting a secular increase of the clustering amplitude. Other explanations would involve large errors in the identification of faint objects as galaxies or a considerable contamination of the counts by very young highly redshifted galaxies as recently proposed by TINSLEY .     

Selection,Statistics and Photometry of Compact Galaxies with Different Instrumental Equipment. Part I

On plates taken with 2 different photographic telescopes compact galaxies in 3 fields near M₃ and M₉₂ were selected. The integral magnitudes and maximum angular diameters of the compacts were determined. The RITCHEY -CHRéTIEN telescope of the FIGL Observatory for Astrophysics (FOA) with a focal ratio of 1:8.3 has a scale of 1 mm = 16.3, while the Tautenburg SCHMIDT with 1:3.2 has a scale of 1 mm ≌ 52°. From the selection statistics for both telescopes results nearly the same number of objects (50) up to 18^m.5 in V in a field of 1.5□°.60% of these objects are identical. An integral photometry on B plates of the same limiting magnitude from both telescopes leads to nearly the same brightness of objects, while they are o^m.5 fainter on FOA V plates. Because of its smaller focal ratio this telescope does not record the halo parts of the compacts. This is clearly demonstrated by the maximum equidensitometric diameters which on FAO plates are on the average only half of those determined on Tautenburg plates. A diameter magnitude diagram is shown.     

Diagnosing southeast tropical Atlantic SST and ocean circulation biases in the CMIP5 ensemble

Warm sea-surface temperature (SST) biases in the southeastern tropical Atlantic (SETA), which is defined by a region from 5°E to the west coast of southern Africa and from 10°S to 30°S, are a common problem in many current and previous generation climate models. The Coupled Model Intercomparison Project Phase 5 (CMIP5) ensemble provides a useful framework to tackle the complex issues concerning causes of the SST bias. In this study, we tested a number of previously proposed mechanisms responsible for the SETA SST bias and found the following results. First, the multi-model ensemble mean shows a positive shortwave radiation bias of ~20 W m^?2, consistent with models’ deficiency in simulating low-level clouds. This shortwave radiation error, however, is overwhelmed by larger errors in the simulated surface turbulent heat and longwave radiation fluxes, resulting in excessive heat loss from the ocean. The result holds for atmosphere-only model simulations from the same multi-model ensemble, where the effect of SST biases on surface heat fluxes is removed, and is not sensitive to whether the analysis region is chosen to coincide with the maximum warm SST bias along the coast or with the main SETA stratocumulus deck away from the coast. This combined with the fact that there is no statistically significant relationship between simulated SST biases and surface heat flux biases among CMIP5 models suggests that the shortwave radiation bias caused by poorly simulated low-level clouds is not the leading cause of the warm SST bias. Second, the majority of CMIP5 models underestimate upwelling strength along the Benguela coast, which is linked to the unrealistically weak alongshore wind stress simulated by the models. However, a correlation analysis between the model simulated vertical velocities and SST biases does not reveal a statistically significant relationship between the two, suggesting that the deficient coastal upwelling in the models is not simply related to the warm SST bias via vertical heat advection. Third, SETA SST biases in CMIP5 models are correlated with surface and subsurface ocean temperature biases in the equatorial region, suggesting that the equatorial temperature bias remotely contributes to the SETA SST bias. Finally, we found that all CMIP5 models simulate a southward displaced Angola–Benguela front (ABF), which in many models is more than 10° south of its observed location. Furthermore, SETA SST biases are most significantly correlated with ABF latitude, which suggests that the inability of CMIP5 models to accurately simulate the ABF is a leading cause of the SETA SST bias. This is supported by simulations with the oceanic component of one of the CMIP5 models, which is forced with observationally derived surface fluxes. The results show that even with the observationally derived surface atmospheric forcing, the ocean model generates a significant warm SST bias near the ABF, underlining the important role of ocean dynamics in SETA SST bias problem. Further model simulations were conducted to address the impact of the SETA SST biases. The results indicate a significant remote influence of the SETA SST bias on global model simulations of tropical climate, underscoring the importance and urgency to reduce the SETA SST bias in global climate models.     

Experimental determination of turbulent fluxes over the heterogeneous LITFASS area: Selected results from the LITFASS-98 experiment

Summary ?During the LITFASS-98 experiment, local flux measurements were performed over five different types of underlying surface (grass, barley, triticale, pine forest, water) in a heterogeneous landscape using eddy covariance and profile techniques over a three week time period in June, 1998. Estimates of the area-integrated sensible heat flux during daytime were obtained from continuous measurements with a large aperture scintillometer (LAS) along a 4.7 km path. The calculation of a mean diurnal cycle of the fluxes during the experiment revealed significant differences between the main land use classes. A land-use weighted average of the sensible heat flux was found to be in good agreement with the LAS based estimate, which in turn was supported by other regionally integrated flux estimates from budget considerations and aircraft measurements for a few case studies. The profiles of turbulent quantities measured along a 99 m-tower significantly deviate from “idealised” profiles measured over homogeneous terrain. Peculiarities in the profile structure could be attributed to the heterogeneity of the terrain, namely to the differences in the surface characteristics of the footprint areas for the different tower levels. Received June 6, 2001; revised January 15, 2002; accepted April 4, 2002