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This comprehensive volume summarizes current knowledge of the Jovian system, in view of recent scientific developments regarding the Galileo spacecraft, the Galileo probe, the Cassini spacecraft, the Hubble Space Telescope, and numerous ground-based and theoretical studies. Chapters by recognized authorities cover all aspects of Jupiter, its satellites and magnetosphere.

This comprehensive volume summarizes current knowledge of the Jovian system, in view of recent scientific developments regarding the Galileo spacecraft, the Galileo probe, the Cassini spacecraft, the Hubble Space Telescope, and numerous ground-based and theoretical studies. Chapters by recognized authorities cover all aspects of Jupiter, its satellites and magnetosphere.

This textbook begins with a description of the Earth's plasma environment, followed by the derivation of single particle motions in electromagnetic fields, with applications to the Earth's magnetosphere. Also discussed are the origin and effects of collisions and conductivities, formation of the ionosphere, magnetospheric convection and dynamics, and solar wind-magnetosphere coupling.The second half of the book presents a more theoretical foundation of plasma physics, starting with kinetic theory. Introducing moments of distribution function permits the derivation of the fluid equations, followed by an analysis of fluid boundaries, with the Earth's magnetopause and bow shock as examples, and finally, fluid and kinetic theory are applied to derive the relevant wave modes in a plasma.This revised edition seamlessly integrates new sections on magnetopause reconstruction, as well as instability theory and thermal fluctuations based on new developments in space physics. Applications such as the important problems of collisionless reconnection and collisionless shocks are covered, and some problems have also been included at the end of each chapter.

Geomagnetic fields arise from a variety of electric current sources. The main, dipolar field results from currents in the Earth's outer core. Dynamo currents, driven by motion of the Earth's ionosphere, generate daily surface field variations, and the Sun's activity modifies the Earth's magnetosphere, producing storm currents on a global scale. Using a minimum of mathematics, and without sacrificing the depth of coverage, the author presents the geomagnetic source fields. Details of measurement methods and a thorough review of the societal impact and use of geomagnetic fields complete the main text. The book concludes with appendices that summarise the necessary background mathematics, provide a comprehensive list of geomagnetic information, and detail geomagnetic utility computer programs. With its refreshing presentation, Introduction to Geomagnetic Fields will appeal to graduate students and researchers seeking an understanding of these natural phenomena.

Alfven waves permeate the universe. They have been observed in the Sun, in the magnetosphere, as low frequency fluctuations in the Earth's magnetic field, and they are easily generated in laboratory plasmas. Alfven waves serve as a useful diagnostic tool to probe plasma conditions in both space and laboratory plasmas. In the quest for nuclear fusion they have been used with spectacular success to heat tokamak plasmas to temperatures exceeding 50 million Kelvin. This book aims to provide an introduction to the physics of Alfven wave propagation for postgraduate physicists and astrophysicists who are entering research on laboratory or space plasmas. In the early chapters the basic properties of Alfven waves are derived for homogeneous plasmas, using the ideal magnetohydrodynamic fluid equations. The essential differences between torsional and compressional wave types are highlighted by an examination of phase and group velocity surfaces, and by a discussion of recent experimental results obtained with small, 'point-source', antennae. Later chapters deal with cylindrical plasmas, Alfven waves in a plasma with two or more ion species, effects of plasma current, resistive damping and inhomogeneous plasmas. There are also two chapters about numerical and experimental techniques, topics which are often neglected in other books.

The reconnection of magnetic fields is one of the most fascinating processes in plasma physics, responsible for phenomena such as solar flares and magnetospheric substorms. The concept of reconnection has developed through recent advances in exploring the magnetospheres of the Sun and Earth through theory, computer simulations and spacecraft observations. The great challenge in understanding it stems from balancing the large volumes of plasma and magnetic fields involved with the energy release with the physical mechanism which relies on the strongly localized behavior of charged particles. This book, edited by and with contributions from leading scientists in the field, provides a comprehensive overview of recent theoretical and observational findings concerning the physics of reconnection and the complex structures that may give rise to, or develop from, reconnection. It is intended for researchers and graduate students interested in the dynamics of plasmas.

Magnetohydrodynamics describes dynamics in electrically conductive fluids. These occur in our environment as well as in our atmosphere and magnetosphere, and play a role in the sun's interaction with our planet. In most cases these phenomena involve turbulences, and thus are very challenging to understand and calculate. A sound knowledge is needed to tackle these problems. This work gives the basic information on turbulence in nature, comtaining the needed equations, notions and numerical simulations. The current state of our knowledge and future implications of MHD turbulence are outlined systematically. It is indispensable for all scientists engaged in research of our atmosphere and in space science.

Magnetohydrodynamics describes dynamics in electrically conductive fluids. These occur in our environment as well as in our atmosphere and magnetosphere, and play a role in the sun's interaction with our planet. In most cases these phenomena involve turbulences, and thus are very challenging to understand and calculate. A sound knowledge is needed to tackle these problems. This work gives the basic information on turbulence in nature, comtaining the needed equations, notions and numerical simulations. The current state of our knowledge and future implications of MHD turbulence are outlined systematically. It is indispensable for all scientists engaged in research of our atmosphere and in space science.

This textbook deals with the requirements of space physics. The first part starts with a description of the Earth's plasma environment, followed by a derivation of single particle motions in electromagnetic fields, with applications to the Earth's magnetosphere. Then the origin and effects of collisions and conductivities, formation of the ionosphere, magnetospheric convection and dynamics, and solar wind-magnetosphere coupling are discussed.The second part of the book presents a more theoretical foundation of plasma physics, starting from kinetic theory. Introducing moments of the distribution function permits derivation of the fluid equations, followed by an analysis of fluid boundaries, with the Earth's magnetopause and bow shock as examples. Finally, fluid and kinetic theory are applied to derive the relevant wave modes in a plasma.A representative selection of the many space plasma instabilities and relevant aspects of nonlinear theory is given in a companion textbook, Advanced Space Plasma Physics, by the same authors.

How can the drag coefficient of a car be reduced? What factors govern the variation in the shape of the Earth's magnetosphere? What is the basis of weather prediction? These are examples of problems that can only be tackled with a sound knowledge of the principles and methods of fluid dynamics. This important discipline has applications which range from the study of the large-scale properties of the galaxies to the design of high precision engineering components. This book introduces the subject of fluid dynamics from the first principles. The first eleven chapters cover all the basic ideas of fluid mechanics, explaining carefully the modelling and mathematics needed. The last six chapters illustrate applications of this material to linearised sound and water waves, to high speed flow of air, to non-linear water waves on channels, and to aerofoil theory. Over 350 diagrams have been used to illustrate key points. Exercises are included to help develop and reinforce the reader's understanding of the material presented. References at the ends of each chapter serve not only to guide readers to more detailed texts, but also list where alternative descriptions of the salient points in the chapter may be found. This book is an undergraduate text for second or third year students of mathematics or mathematical physics, who are taking a first course in fluid dynamics.

Geomagnetic fields arise from a variety of electric current sources. The main, dipolar field results from currents in the Earth's outer core. Dynamo currents, driven by motion of the Earth's ionosphere, generate daily surface field variations, and the Sun's activity modifies the Earth's magnetosphere, producing storm currents on a global scale. Using a minimum of mathematics, and without sacrificing the depth of coverage, the author presents the geomagnetic source fields. Details of measurement methods and a thorough review of the societal impact and use of geomagnetic fields complete the main text. The book concludes with appendices that summarise the necessary background mathematics, provide a comprehensive list of geomagnetic information, and detail geomagnetic utility computer programs. With its refreshing presentation, Introduction to Geomagnetic Fields will appeal to graduate students and researchers seeking an understanding of these natural phenomena.

From the Preface: "The Saturn system is the most complex in the universe and this book is to summarize it all: the planet, rings, satellites, the magnetospheres, and the interaction with the interplanetary medium. The effective date of the material is approximately November 1983."

How can the drag coefficient of a car be reduced? What factors govern the variation in the shape of the Earth's magnetosphere? What is the basis of weather prediction? These are examples of problems that can only be tackled with a sound knowledge of the principles and methods of fluid dynamics. This important discipline has applications which range from the study of the large-scale properties of the galaxies to the design of high precision engineering components. This book introduces the subject of fluid dynamics from the first principles. The first eleven chapters cover all the basic ideas of fluid mechanics, explaining carefully the modelling and mathematics needed. The last six chapters illustrate applications of this material to linearised sound and water waves, to high speed flow of air, to non-linear water waves on channels, and to aerofoil theory. Over 350 diagrams have been used to illustrate key points. Exercises are included to help develop and reinforce the reader's understanding of the material presented. References at the ends of each chapter serve not only to guide readers to more detailed texts, but also list where alternative descriptions of the salient points in the chapter may be found. This book is an undergraduate text for second or third year students of mathematics or mathematical physics, who are taking a first course in fluid dynamics.

The reconnection of magnetic fields is one of the most fascinating processes in plasma physics, responsible for phenomena such as solar flares and magnetospheric substorms. The concept of reconnection has developed through recent advances in exploring the magnetospheres of the Sun and Earth through theory, computer simulations and spacecraft observations. The great challenge in understanding it stems from balancing the large volumes of plasma and magnetic fields involved with the energy release with the physical mechanism which relies on the strongly localized behavior of charged particles. This book, edited by and with contributions from leading scientists in the field, provides a comprehensive overview of recent theoretical and observational findings concerning the physics of reconnection and the complex structures that may give rise to, or develop from, reconnection. It is intended for researchers and graduate students interested in the dynamics of plasmas.

From the Preface: "The Saturn system is the most complex in the universe and this book is to summarize it all: the planet, rings, satellites, the magnetospheres, and the interaction with the interplanetary medium. The effective date of the material is approximately November 1983."

An Introduction to Space Plasma Complexity considers select examples of complexity phenomena related to observed plasma processes in the space environment, such as those pertaining to the solar corona, the interplanetary medium, and Earth's magnetosphere and ionosphere. This book provides a guided tour of the ideas behind forced and/or self-organized criticality, intermittency, multifractals, and the theory of the dynamic renormalization group, with applications to space plasma complexity. There is much to be explored and studied in this relatively new and developing field. Readers will be able to apply the concepts and methodologies espoused in this introduction to their own research interests and activities.

This work deals with upper atmosphere physics, the magnetosphere and the solar wind. Some topics covered within these areas are geomagnetic pulsations and plasma waves, storms and substorms in the magnetospheres and auroras.