The continuous stream of particles flowing outward from the Sun is called the solar wind. It mostly consists of electrons and protons with energies usually between 1.5 and 10 ke V. The stream of particles varies in temperature and speed over time. These particles can escape the Sun’s gravity because of their high kinetic energy and the high temperature of the corona. In this book, the authors present current research in the study of the emission, technologies and impact of solar wind. Topics include the possible impact of the astronomical aspects of the violent cyclonic motions in the Earth’s atmosphere; planetary beat, solar wind and terrestrial climate; historical background on Eugene Parker and his conception and formulation of solar wind; solar wind influences on atmospheric processes in winter Antarctica; and experimental and modeling evidences of solar wind energy on the Earth’s atmosphere.
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