Practical pedotransfer functions for estimating the saturated hydraulic conductivity

The saturated hydraulic conductivity k is one of the most important and widely used geotechnical parameters, commonly involved in a diversity of applications. The value of k depends on many factors, which can be divided into three classes: properties of the fluid, pore size distribution, and characteristics of the solid surfaces. Because the latter two are not necessarily constant within a given deposit, the hydraulic conductivity may vary significantly in space. Engineers and scientists need indications about how changing factors may affect the actual k value. In this paper, the authors propose some simple expressions, based on pedologic properties, to estimate the value of k. Using experimental results of their own and taken from the literature, it is shown that the proposed pedotransfer functions can be used for quickly estimating the k value for granular and plastic/cohesive soils. Such expressions can be employed, with a useful chart format, for the preliminary design phase of a project, and also for estimating the range of k values to be anticipated within a given deposit.     

The Channel Tunnel: Geostatistical prediction of the geological conditions and its validation by the reality

Geometric modeling of the geological layers in the Channel Tunnel area employed local variography and kriging for computing meaningful predictions and confidence intervals. The results were used to design the alignment of the tunnel, and tunneling was completed on March 28, 1991, 1 month ahead of the initial schedule. Data from 85 borehole pairs drilled during tunneling enable the geostatistical prediction to be compared with the reality, which is seldom possible. They fully validate the geostatistical approach.     

Amorce de la Sédimentation Synorogénique dans les PyrénéesVarisques. Données Chronologiques; Implications Paléogéographiques

Conodont associations and recent macrofaunal discoveries, allow us to date the beginning of detrital deposits going with the Variscan uplift in the Pyrenean marine basins during the Lower Carboniferous. Thus, the establishing of synorogenic conditions seems to have progressed from the East to the West; there appears the picture of a kind of north-Pyrenean axis already individualized in the wide Cantabrico-Pyrenean foreland.     

Variation ofb values before the Etnean eruption of March 1981

A fissural eruption occurred from the northern flank of Mt. Etna on March 17, 1981, and the associated earthquake activity, recorded by the seismic network operating on the volcano, was carefully examined to detect possible variations ofb values, according to the frequency-magnitude relationship, before the start of the eruption. The analysis of 4000B-type earthquakes was carried out according to the maximum likelihood method. A significant increase in theb value was noticed since the beginning of February 1981, followed by a sharp decrease in the days before the eruption started. The observed variation pattern was related to possible changes on the stress field acting on the volcano.     

Performance and Early Results from the Golf Instrument Flown on the Soho Mission

GOLF in-flight commissioning and calibration was carried out during the first four months, most of which represented the cruise phase of SOHO towards its final L1 orbit. The initial performance of GOLF is shown to be within the design specification, for the entire instrument as well as for the separate sub-systems. Malfunctioning of the polarising mechanisms after 3 to 4 months operation has led to the adoption of an unplanned operating sequence in which these mechanisms are no longer used. This mode, which measures only the blue wing of the solar sodium lines, detracts little from the detection and frequency measurements of global oscillations, but does make more difficult the absolute velocity calibration, which is currently of the order of 20%. Data continuity in the new mode is extremely high and the instrument is producing exceptionally noise-free p-mode spectra. The data set is particularly well suited to the study of effects due to the excitation mechanism of the modes, leading to temporal variations in their amplitudes. The g modes have not yet been detected in this limited data set. In the present mode of operation, there are no indications of any degradation which would limit the use of GOLF for up to 6 years or more.     

Stellar winds and mass loss of a rotating star

The mass loss to be expected from the corona of a rotating F2-star is calculated. The rotation is supposed to be rigid up to a certain distances, as if it were maintained by a strong magnetic field. Dependent on the values of the rotational velocity the mass loss can increase to 26–40% forv _rot up to 200 km s^–1.     

A dynamo scenario for polar and whole-surface starspot generation

Rapidly rotating young (T Tauri, pre-Main-Sequence, and Main-Sequence) stars as well as subgiants seem to show starspots not only at low and middle latitudes, as the Sun, but also at high latitudes and even around the poles. We consider a simple nonlinear Parker migratory dynamo model working in a thin shell in order to investigate how high latitude and polar spots may be produced for different values of the dynamo layer radius and thickness and for various rotation rates. Simple assumptions on the angular velocity gradient and helicity distribution are made according to symmetry properties and recent solar and stellar observations. A recently proposed asymptotic WKB-type approach is used to solve the dynamo problem and its drawbacks and advantages in the solar and stellar contexts are discussed. As a general result, we find that a sizable toroidal field can be produced over a much more extended latitude range than in the Sun, thus explaining in a natural way the occurrence of activity from the poles to the equator in such stars. Our approach complements that proposed by Schüssler et al. (1996) which is focused on the instability and emergence of the azimuthal flux tubes, as well as the analyses based on a dynamo working over an extended part of the stellar convective envelope (Moss, Tuominen, and Brandenburg, 1991; Moss et al., 1995).