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Physics of the Inner Heliosphere II pp 45–133Cite as

Kinetic Physics of the Solar Wind Plasma

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Part of the book series: Physics and Chemistry in Space ((SPACE,volume 21))

Abstract

The interplanetary medium has been continuously explored for more than two decades and substantial progress has been made, both with regard to in situ measurements and a theoretical understanding of the solar wind. Concurrently, measurement techniques for remote sensing of its source regions in the solar corona by means of photons covering the full electromagnetic spectrum from γ-rays to radar have also become mature. The results obtained have greatly improved and corroborated our knowledge about the solar wind from the very coronal base to several solar radii and further out into interplanetary space (see the reviews [8.15, 66–68, 76, 109, 119, 120, 126, 131, 134, 215, 245] and [8.22, 23, 26, 286, 288]). However, even after completion of the Helios mission there remains an important but poorly explored region in the inner heliosphere below 0.3 AU to be investigated and, of course, the wide space out of the ecliptic plane and above the solar poles. Whereas a solar probe, the feasibility of which has already been demonstrated [8.239], may possibly be realized in the far future, the out-of-ecliptic mission [8.199] is soon to become reality and will certainly help to comprehend better the three-dimensional structure of the heliosphere.

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  1. Eckart Marsch
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Marsch, E. (1991). Kinetic Physics of the Solar Wind Plasma. In: Schwenn, R., Marsch, E. (eds) Physics of the Inner Heliosphere II. Physics and Chemistry in Space, vol 21. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-75364-0_3

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  • DOI: https://doi.org/10.1007/978-3-642-75364-0_3

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