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Ohne Zusammenfassung     

Further notes on the geology of the betic of Málaga,the Subbetic,and the zone between these two units,in the region of Vélez Rubio (southern Spain)

The stratigraphy of Betic of Málaga and of Subbetic near Vélez Rubio is given. No major tectonic movement took place between Paleozoic and Oligo-Miocene in the area of deposition of the Betic of Málaga and neighbourhood. The geology and formations of the narrow zone between Betic of Málaga and Subbetic are described. Nappe movement of the Betic of Málaga is older than the thrusting of Subbetic over Prebetic. Age of the former movement and origin of major tectonic units are tested on the characteristics of a pre-Orbulina marl formation and on the distribution of the detritus contained in this formation.

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Zusammenfassung Die Stratigraphie des Betikums von Málaga, des Subbetikums und der zwischen beiden Einheiten liegenden Zone wird aus dem Gebiet von Vélez Rubio beschrieben.Größere tektonische Bewegungen haben zwischen Paläozoikum und OligoMiozän im Ablagerungsgebiet des Betikums von Málaga und in der näheren Umgebung nicht stattgefunden. Die Deckenbewegung des Betikums von Málaga ist älter als die Überschiebung des Subbetikums über das Präbetikum. Das Alter der Deckenbewegung und der Ursprung der größeren tektonischen Einheiten werden an Hand der Merkmale einer Prä-Orbulina Mergel-Einheit und an Hand der Verbreitung des in dieser Einheit enthaltenen Schutts überprüft.

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Résumé Les auteurs exposent la stratigraphie du Bétique de Málaga et du Subbétique dans les environs de Vélez Rubio. Aucun mouvement tectonique important n'a eu lieu entre le Paléozoïque et l'Oligo-Miocène dans l'aire sédimentaire du Bétique de Málaga et les régions limitrophes. Les formations de l'étroite zone comprise entre Bétique de Málaga et Subbétique sont étudiées, ainsi que leur relations mutuelles. Le mouvement de nappe du Bétique de Málaga est plus ancien que le chevauchement du Subbétique sur le Prébétique. L'âge de celui-là, ainsi que l'origine des unités tectoniques principales sont examinés en utilisant les caractéristiques d'une formation d'âge pré-Orbulina ainsi que la répartition des débris dérivés de ces unités tectoniques qu'elle contient.

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Folgerungen für die Entstehung der Basalte aus dem speziellen Auftreten der Pyroxene in diesen Gesteinen

Zusammenfassung Die früheren Angaben über die Pyroxenführung, besonders über den Gehalt an rhombischem Pyroxen, wurden in den Basalten der südwestlichen Ausläufer des Vogelsberges überprüft. Es kann in Abhängigkeit vom SiO₂-Gehalt dieser Gesteine eine Beziehung über die Zusammensetzung der Basalte und die Art der auftretenden Pyroxene aufgestellt werden. Vereinfacht ergibt sich, daß die Olivinbasalte keinen rhombischen Pyroxen in der Grundmasse führen - abgesehen von den Olivinknollen - und die Gesteine mit Bronzitführung dem gabbrodioritischen bzw. dioritischen Magmentyp angehören. Daneben kommt Pigeonit in weiter Verbreitung vor. Diese Befunde unterstützen die Auffassung, daß die Olivinknollen der Basalte Reste von assimilierten Peridotiten sind. die dem basaltischen primären Magma zugefügt werden. Dadurch wird ein Hinweis auf den Ort der Bildung der basaltischen Magmen gegeben.     

Drop shape and erosivity part I: Experimental set up,theory, and measurements of drop shape

Simulated raindrops falling in still air have a shape that is mainly determined by surface tension and hydrostatic pressure. Drops released from capillary tips show an initial shape variation ranging from prolate to oblate but eventually this oscillation is damped. At terminal velocity drops have attained equilibrium and have an oblate shape. Measurements of the shape of simulated rain drops produced by capillary tubes were made using a simple, newly-developed photographic set up. The measurements showed that models describing the oscillation frequency and amplitude of drops falling at terminal velocity can also be applied to the simulated drops. A comparison is made between the shape of raindrops in natural storms and simulated drops. Recommendations are given regarding fall heights in simulation in relation to the drop shape in nature.     

Creep processes in landslides

Displacement of landslide blocks after initial slope failure can be very slow. In most cases movement of the blocks is attributed to sliding along a well-defined slip surface. It is discussed here whether, in addition to these so-called plastic movements, (continuous) creep processes are involved in the slow displacement. The study was carried out in the downstream part of the Bonne valley in the French Alps, where landslide complexes have developed in varved clay material. Displacements of landslide blocks were measured during a period of three years. Inclinometer measurements in flexible tubes showed that a creep zone developed above the slip surface in a zone about 1 m thick. These field observations on creep processes were supported by soil mechanical analysis. Threshold values for creep found in the laboratory nearly coincide with threshold values calculated from a field creep model developed by Ter-Stepanian. During the measuring period ±15 per cent of the displacement of the blocks possibly occurred via continuous creep.     

Structure of the solar granulation

The structure of the solar granulation has been analysed using computer-processed images of two very high resolution (0.25) white-light pictures obtained at the Pic-du-Midi Observatory.The narrow dispersion in the distribution of granule sizes is not confirmed. On the contrary, it is found that the number of granules increases continuously toward smaller scales; this means that the solar granulation has no characteristic or mean scale. Nevertheless, the granules appear to have a critical scale of 1.37, at which drastic changes in the properties of granules occur; in particular the fractal dimension changes at the critical scale. The granules smaller than this scale could be of turbulent origin.     

Self-regulated star formation and the evolution of stellar systems

In this paper we estimate the star formation efficiency using the assumption that star formation continues until the radiation pressure disrupts the cloud. The results that in the case of low/mediummass star formation the efficiency could be about five times higher than in the case of high-mass star formation.For a three-component star-forming system (low/medium-mass stars, high-mass stars, gas) we investigate the temporal behaviour and the final star formation efficiency. We can show that the efficiency in 10⁴ M clouds is higher than in 10⁶ M clouds. This supports our view that bound stellar systems form from medium-mass clouds, whereas OB associations form in the cores of giant molecular clouds. Furthermore, the effect of induced high-mass star formation may cause a change of the mass spectrum during the formation of an OB association.Paper presented at a Workshop on The Role of Dust in Dense Regions of Interstellar Matter, held at Georgenthal, G.D.R., in March 1986.     

Explicit expression and regularization of the harmonic reproducing kernels for the earth's ellipsoid

The reproducing kernel functions and the integral formulae involving the solutions of the fixed gravimetric boundary value problems for the earth's ellipsoid are investigated in a suitable polar coordinate system defined on the boundary ellipsoid. The infinite series expressions of the reproducing kernel functions are represented explicitly up to the square of the first excentricity of the boundary surface. The obtained results show that the reproducing kernel functions for the earth's ellipsoid are, in contrast to the case of the spherical boundary, inhomogeneous and anisotropic. Moreover, the anisotropy is stronger near the pole. Subsequently the kernel functions are regularized in order to overcome the weak singularity of the integrals.