Description

The magnetosphere is the region where cosmic rays and the solar wind interact with the Earth's magnetic field, creating such phenomena as the northern lights and other aurorae. The configuration and dynamics of the magnetosphere are of interest to planetary physicists, geophysicists, plasma astrophysicists, and to scientists planning space missions. The circulation of solar wind plasma in the magnetosphere and substorms have long been used as the principle paradigms for studying this vital region. Charles F. Kennel, a leading scientist in the field, here presents a synthesis of the convection and substorm literatures, and an analysis of convection and substorm interactions; he also suggests that the currently accepted steady reconnection model may be advantageously replaced by a model of multiple tail reconnection events, in which many mutually interdependent reconnections occur. Written in an accessible, non-mathematical style, this book introduces the reader to the exciting discoveries in this fast-growing field.

Reviews

"... a well-supported claim of a shift in paradigm from the old quasi-steady picture of convection to a new, much more dynamic one .... Primarily, however, it provides enjoyment and stimulation for the educated reader, and I highly recommend it to all colleagues interested in the topic." --Eos

Product Details

432 pages; 35 illus; 6-1/8 x 9-1/4; ISBN13: 978-0-19-508529-7ISBN10: 0-19-508529-9

About the Author(s)