Flow And Creep In The Solar System Observations Modeling And Theory

The NATO ASI held in the Geophysical Institute, University of Alaska Fairbanks, June 17-28, 1991 was, we believe, the first attempt to bring together geoscientists from all the disciplines related to the solar system where fluid flow is a fundamental phenomenon. The various aspects of flow discussed at the meeting ranged from the flow of ice in glaciers, through motion of the solar wind, to the effects of flow in the Earth's mantle as seen in surface phenomena. A major connecting theme is the role played by convection. For a previous attempt to review the various ways in which convection plays an important role in natural phenomena one must go back to an early comprehensive study by 1. Wasiutynski in "Astro physica Norvegica" vo1. 4, 1946. This work, little known now perhaps, was a pioneering study. In understanding the evolution of bodies of the solar system, from accretion to present-day processes, ranging from interplanetary plasma to fluid cores, the understanding of flow hydrodynamics is essentia1. From the large scale in planetary atmospheres to geological processes, such as those seen in magma chambers on the Earth, one is dealing with thermal or chemical convection. Count Rumford, the founder of the Royal Institution, studied thermal convection experimentally and realized its practical importance in domestic contexts.

In this reference for geologists, 20 contributions from international scientists discuss the analytical, physical, and numerical modeling of tectonic processes. A sampling of topics includes types of transpressional and transtensional deformation, modeling of anisotropic grain growth in minerals, salt tectonics and sedimentation along Atlantic margins, and new apparatus for thermomechanical analogue modeling. The text is accompanied throughout by b&w illustrations. Annotation c. Book News, Inc., Portland, OR (booknews.com)

Sixty-five papers cover a wide range of topics from engineering applications to theoretical developments in the areas of embankment and slope stability, underground cavity design and mining; dynamic analysis, soil and structure interaction, and coupled processes and fluid flow.

Written as both a textbook and a handy reference, this text deliberately avoids complex mathematics assuming only basic familiarity with geodynamic theory and calculus. Here, the authors have brought together the key numerical techniques for geodynamic modeling, demonstrations of how to solve problems including lithospheric deformation, mantle convection and the geodynamo. Building from a discussion of the fundamental principles of mathematical and numerical modeling, the text moves into critical examinations of each of the different techniques before concluding with a detailed analysis of specific geodynamic applications. Key differences between methods and their respective limitations are also discussed - showing readers when and how to apply a particular method in order to produce the most accurate results. This is an essential text for advanced courses on numerical and computational modeling in geodynamics and geophysics, and an invaluable resource for researchers looking to master cutting-edge techniques. Links to supplementary computer codes are available online.

I have been asked by Professor Kikuchi to write a foreword for this interesting book on Dusty Plasmas and other electrical phenomena. This was a somewhat daunting task due to the wide range of topics covered. In what follows I have attempted to summarize most of these topics; for this purpose I have divided them into four groups, namely (a) Dusty Plasmas, (b) The Electrical Environment, (c) Lightning and (d) The Noise Environment. I hope that I have succeeded. in indicating that each section contains much that is of great interest. It is perhaps unnecessary for me to point out that the book contains subjects which are at an exciting and important stage in their development. (a) Dusty Plasmas The subject of dusty plasmas is one of great interest. Dust particles in interplanetary space, within comets, in inter-stellar space and at ever greater distances will in general be charged. The plasma environment will ensure this, bombarding electrons will charge up the particle until it assumes a "floating potential," although time variation can occur. Ultra violet radiation can cause photoemission and in certain cases field emission is a possibility. The motion of the particles will be determined by electric and magnetic fields together with gravity. If the density of charged grains becomes sufficiently high the grains will interact with each other and collective behaviour will ensue. This newly evolving subject entails the study of all kinds of plasma waves.

The final orbit of Venus by the Magellan spacecraft in October 1994 brought to a close an exciting period of Venus reconnaissance and exploration. The scientific studies resulting from data collected by the Magellan, Galileo, and Pioneer missions are unprecedented in their detail for any planet except Earth. Venus II re-evaluates initial assessments of Venus in light of these and other spacecraft missions and ground-based observations conducted over the past 30 years. More than a hundred contributors summarize our current knowledge of the planet, consider points of disagreement in interpretation, and identify priorities for future research. Topics addressed include geology, surface processes, volcanism, tectonism, impact cratering, geodynamics, upper and lower atmospheres, and solar wind environment. The diversity of the coverage reflects the interdisciplinary nature of Venus science and the breadth of knowledge that has contributed to it. A CD-ROM developed by the Jet Propulsion Laboratory accompanies the book and incorporates text, graphics, video, software, and various digital products from selected contributors to the text. A multimedia interface allows users to navigate the text and the extensive databases included on the disk. Venus II is the most authoritative single volume available on the second planet. Its contents will not only help shape the goals of future Venus missions but will also enhance our understanding of current Mars explorations.

This volume summarises our present understanding of the formation of passive continental margins and their ocean-continent transitions. It outlines the geological, geophysical and petrological observations that characterize extensional systems, and how such observations can guide and constrain dynamic and kinematic models of continental lithosphere extension, breakup and the inception of organized sea-floor spreading.