As a star in the universe, the Sun is constantly releas- cover a wide range of time and spatial scales, making ing energy into space, as much as ?. ? erg/s. Tis observations in the solar-terrestrial environment c- energy emission basically consists of three modes. Te plicated and the understanding of processes di?cult. ?rst mode of solar energy is the so-called blackbody ra- In the early days, the phenomena in each plasma diation, commonly known as sunlight, and the second region were studied separately, but with the progress mode of solar electromagnetic emission, such as X rays of research,...

Since the early 1990's, a large number of new data sets have become available as a result of both the highly successful ISTP satellite missions and extensive ground-based observations. The advance of computer networks has led to the effective exchange and treatment of these data sets, improving our ability to study dynamic behavior in the Earth's electromagnetic environment. Attempts have also been made to compare in an orchestrated fashion computer simulations with realistic boundary conditions resulting from in-situ observations in space. The Fourth International Conference on Substorms...

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...

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...

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...