Soil/Geotextile Interface Behaviour in Direct Shear and Pullout Movements

This paper deals with soil/reinforced geotextile interface behaviour in direct shear and pullout movements. A soil/geosynthetic direct shear apparatus, developed in accordance to EN ISO 12957-1 (2004) and ASTM D5321-92 (1992) standards, is presented. Some details of the test (like: specimen fixation, influence of the vertical stress on the registered horizontal force, type of test and measurement of the vertical displacement) are discussed and modifications in the test procedures are adopted. Then, the reinforced geotextile and the residual soil of granite used in the research are described. The behaviour of soil/geosynthetic interface in direct shear is characterized based on modified direct shear tests and maximum interface shear stress is determined at peak and residual for a confining stress of 50 kPa. The modification in the pullout test apparatus described by Lopes and Ladeira (1996a; 1996b) and by Lopes and Lopes (1999) are noticed. The behaviour of soil/geosynthetic interface in pullout is characterized based on pullout tests performed, in accordance EN 13738 (2004), and interface shear stress at maximum pullout force is defined for a confining stress of 50 kPa. Finally, the values of interface coefficient at soil/geosynthetic interface are obtained in direct shear and in pullout and then compared. The main conclusions that can be outlined from the present study are the following: modifications should be made to EN ISO 12957-1 (2004) standard, namely in what concerns the dependence of the measured horizontal force from the vertical stress, the difficulties to perform constant area direct shear test with the lower half box filled with soil and on the measurement of the vertical displacement of the load plate; on the contrary to which is normally accepted the characteristics of the behaviour of soil/geosynthetic interface in pullout, when the geosynthetic has a full plane contact area with the soil, are not able to be obtained based on results of direct shear tests, as in this type of tests the contribution of the geosynthetic deformation on the characteristics of the interface in pullout is not considered.     

The Mineral Adsorption and The Application of a Metamorphic Felsic Rock as Aggregate in Asphalt Pavements

Geotechnical and Geological Engineering - The aggregates consist approximately 85% of the total volume in asphalts pavements, and their properties influence directly their behavior. Therefore, it...     

Astrophysical Jet Simulations: Comparing Different Numerical Methods

High resolution Godunov-type methods have gained increasing popularity in the last decade due to their ability in modelling highly supersonic flows. Most of these shock-capturing schemes are based on the solution of the Riemann problem between discontinuous data at each cell's interface. The purpose of this work is to investigate the role played by different Riemann solvers in the evolution of a supersonic jet. Morphology, dynamics, conservation properties and cocoon characteristics are examined for the four different cases presented.     

Hydrodynamical simulations of Galactic fountains – I. Evolution of single fountains

The ejection of the gas out of the disc in late-type galaxies is related to star formation and is due mainly to Type II supernovae. In this paper, we studied in detail the development of the Galactic fountains in order to understand their dynamical evolution and their influence on the redistribution of the freshly delivered metals over the disc. To this aim, we performed a number of 3D hydrodynamical radiative cooling simulations of the gas in the Milky Way where the whole Galaxy structure, the Galactic differential rotation and the supernova explosions generated by a single OB association are considered. A typical fountain powered by 100 Type II supernovae may eject material up to ∼2 kpc which than collapses back mostly in the form of dense, cold clouds and filaments. The majority of the gas lifted up by the fountains falls back on the disc remaining within a radial distance  Δ R = 0.5 kpc  from the place where the fountain originated. This localized circulation of disc gas does not influence the radial chemical gradients on large scale, as required by the chemical models of the Milky Way which reproduce the metallicity distribution without invoking large fluxes of metals. Simulations of multiple fountains fuelled by Type II supernovae of different OB associations will be presented in a companion paper.     

Process-based 2DH morphodynamic modeling of tidal inlets: A comparison with empirical classifications and theories

The economical and ecological importance of tidal inlets has fostered the development of empirical tools for inlet management during the last century. This study aims at confronting these empirical theories with results obtained with a process-based numerical model, MORSYS2D. This 2DH morphodynamic modeling system is applied to an idealized tidal inlet/lagoon system with different combinations of significant wave height, tidal range and tidal prism. The numerical model predictions are compared to the empirical models of Hayes, Bruun, O'Brien and FitzGerald and to morphologies observed at natural tidal inlets. The results present good accordance with observations as well as with some key behaviors predicted with the empirical theories. The predicted morphologies satisfy the relation of O'Brien between the tidal prism and the cross-sectional area, the model reproduces the conceptual model of sand by-passing by ebb-tidal delta breaching of FitzGerald and the classifications of Hayes and Bruun are generally respected. However, some inconsistencies between model results and Hayes classification highlight the limitations of applying this classification, which only considers the yearly-averaged significant wave height and tidal range, to a single tidal inlet case.     

The dynamics of velocity fluctuations in the solar wind – I. Coronal mass ejections

In this paper we present a simple, analytic model for the dynamical evolution of supersonic velocity fluctuations at the base of the ambient solar wind. These fluctuations result in the formation of dense working surfaces that travel down the wind. It is shown how the initial parameters of the fluctuations (velocity, density and duration) are related to the characteristics of the working surfaces far from the Sun (for instance at the Earth). We apply the model to the evolution of the coronal mass ejections in the IP medium, finding that the model is in good agreement with satellite observations of these phenomena, thus providing physical insight into their dynamical evolution. Our model may contribute to future 'space weather forecasting' on the Earth, based on detailed satellite monitoring of the solar corona.