Abstract
This review will concentrate on the interpretation of recent observations pertaining to the chemical composition and dynamical behavior of the solar wind plasma.
The solar wind helium content has been determined in several independent series of observations; the long-term average abundance of helium relative to hydrogen is close to 4.5% by number. This ratio is lower than that usually given for the solar photosphere, possibly implying a separation of ions with different charge-to-mass ratios in the coronal expansion. Such a separation could result from gravitational settling of heavy coronal ions. A helium-rich plasma has been frequently observed some hours after the passage of a flare-associated interplanetary shock wave; this plasma has been tentatively identified as material ejected from the chromosphere or low corona by the flare. The isotope 3He has been observed by two independent techniques and found to be ~ 103 times less abundant than 4He. Several ions of 160 have also been identified in the solar wind, with varying total abundance. The observed ionization state of oxygen can be related to the coronal temperature.
Recent observations have established the ranges and average values of the fluid parameters used to describe the solar wind. Attempts to explain observed solar wind temperatures within the framework of fluid models of the coronal expansion require hypotheses of dynamic processes which deposit or redistribute energy in inteplanerary space. Some of the conflicting ideas regarding these processes will be discussed.
The transient behavior of the solar wind has attracted increasing observational and theoretical attention. Numerous observations of interplanetary shock waves indicate that the typical shock wave propagates at ~ 500 km sec−1 at 1 AU. In addition to this extreme class of transient phenomena, other long-term patterns of spatial or temporal variation have been found. The common occurrence of such patterns raises questions as to the applicability of the usual spherically symmetric, steady-state models of the coronal expansion in the interpretation of many solar wind observations.
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Hundhausen, A.J. (1972). Composition and Dynamics of the Solar Wind Plasma. In: Dyer, E.R. (eds) Solar-Terrestrial Physics/1970. Astrophysics and Space Science Library, vol 29. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3693-5_14
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