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3 185 kr
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The 4th International Conference on Substorms (ICS-4) was held at Lake Hamana, Japan on March 9-13, 1998. This volume represents a snapshot of substorm research as of 1998. The proceedings address the following key questions: what are the major expansion phase activities seen in various regions?; what triggers the substorm expansion onset?; what are the roles of waves and microscopic processes in large-scale substorm processes?; what is the relationship between global convection and substorms?; and what is the role of the inner magnetosphere during substorms? For each of the five key questions, the status of observational and modelling efforts in the field is presented in the invited and contributed papers. This volume will foster communication between magnetospheric and high-latitude ionospheric physicists and those scientists who are working primarily in the area of the thermosphere and low-latitude ionosphere.
537 kr
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In the past two decades a succession of direct observations by satellites, and of extensive computer simulations, has led to the realization that the polar ionosphere plays a principal role in large-scale magnetospheric processes - a manifestation of the physics linkage involved in solar-terrestrial interactions. Spatial/temporal variations in high-latitude electromagnetic phenomena, such as dynamic aurorae, electric fields and currents, have proved to be extremely complex. Now the challenge is to comprehend the vast amount of complicated measurements made in this magnetosphere-ionosphere sysstem of the Earth. This book addresses the electrical coupling between the hot, but dilute, magnetospheric plasma and the cold, but dense, plasma in the ionosphere. In five major chapters, this book presents: - basic properties of magnetosphere-ionosphere coupling; - morphology of electric fields and currents at high latitudes; - global modeling of magnetosphere-ionosphere coupling; - modeling of ionospheric electrodynamics; - current issues, such as auroral particle acceleration, substorms, penetration of high-latitude fields into low latitudes.
3 720 kr
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As a star, the sun is continuously emitting an enormous amount of energy 33 into space, up to as much as 3. 9 X 10 erg/ s. This energy emission consists of three modes. Almost all the energy is emitted in the form of the familiar black-body radiation, commonly called sunlight. Although the amount of energy emitted is small, the sun also emits x rays, extreme ultraviolet (EUV), and UV radiations, which are absorbed above the earth's stratosphere. These constitute the second mode of solar energy, separate from the black-body radiation that penetrates the lower layers of the atmosphere. The sun has another important mode of energy emission in which the energy is carried out by charged particles. These particles have a very wide range of energies, from less than I keY to more than I GeV. Because of this wide range, it is convenient to group them into two components: particles with energies greater than 10 keY and the lower-energy particles. The former are generally referred to as solar protons or solar cosmic rays; their emission is associated with active features on the sun. Their interaction with the atmosphere is similar to that of the x ray and EUV radiation. Low-energy particles constitute plasma, a gas of equal numbers of positive and negative particles. Actually, this plasma is the outermost part of the solar atmosphere, namely the corona, which blows out continuously . For this reason, the plasma flow is called the solar wind.
Del 126 - Astrophysics and Space Science Library
Solar Wind — Magnetosphere Coupling
Häftad, Engelska, 2011
1 068 kr
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This monograph is the outgrowth of an AGU (American Geophysical Union) Chapman Conference on Solar Wind-Magnetosphere Coupling, and it contains most of the formal papers presented at the conference including the summary panel. The conference was held on February 12-15,1985 at the Jet Propulsion Laboratory of the California Institute of Technology in Pasadena, California, U.S.A. It was attended by over 150 scientists from most of the nations active in space research. The purpose of the conference was to bring together scientists from all areas of solar-terrestrial physics, both theoretical and experimental, in order to focus attention on the solar wind-magnetosphere coupling problem, to provide a timely forum for the exchange of ideas, and to promote interdisciplinary collaboration. The conference agenda consisted of eight sessions: six topical, one poster, and one summary. The topical sessions were "Solar Wind and Geomagnetic Activity," "AM PTE Mission," "Solar Wind and Polar Cusp," "Auroral Zone and Polar Cap," "Solar Wind and Magnetotail," and "Theoretical Modeling and Simulations." The conference concluded with a two-hour summary panel discussion which attempted to provide an assessment of the progress that has been made as well as underscore the problems, old and new, which remain unanswered. Sydney Chapman (1889-1970) was one of the early pioneers in the study of the influence of the sun and magnetosphere on the earth's upper atmosphere, and it was most appropriate that this conference be one in the AGU series named in his honor.