Convection and Substorms

Convection and substorms are magnetospheric phenomena used as paradigms for the study of the magnetosphere. This book presents a synthesis of the literature on convection and substorms, an analysis of their interactions, and proposes a new model for reconnection. All scientists working in solar-terrestrial physics will find this book invaluable. It includes a comprehensive bibliography.

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The magnetosphere is the region in which the solar wind interacts with the Earth's magnetic field, the zone which screens the Earth from most of the harmful cosmic rays which daily bombard it. The Aurora Borealis, or Norhun lights, other such phenourena result from the interaction of particles in the solar wind and the magnetosphere.

Planetary physicists, geophysicists, plasma astrophysicists, and scientists involved with astronautics all have a primary interest in the configuration and dynamics of the magnetosphere, and much research is devoted to convection (the circulation of solarwind plastma in the magnetiosphere) and substorms, which are linked to the aurorae and thought to stimulate convection. In this book, one of the leading scientists in the field presents a synthesis of current knowledge on convection and substorms and proposes that the
Planetary physicists, geophysicists, plasma astrophysicists, and scientists involved with astronautics all have a primary interest in the configuration and dynamics of the magnetosphere, and much research is devoted to convection (the circulation of solarwind plastma in the magnetiosphere) and substorms, which are linked to the aurorae and thought to stimulate convection. In this book, one of the leading scientists in the field presents a synthesis of current knowledge on convection and substorms and proposes that the steady reconnection model be replaced by a model of multiple tail reconnection events, in which many mutually interdependent reconnections occur.