Observed Properties of the Slow Solar Wind

Computer Science – Sound

Scientific paper

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2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma, 2169 Solar Wind Sources

Scientific paper

The source of the slow solar wind is poorly understood, in part because observations of its properties have led to conflicting phenomenological views. To provide a sound basis for a synthesis view and, ultimately, for a successful physical model, the observed properties are reviewed with minimal reference to interpretation. Slow wind properties can be sorted into three categories according to scale size. At large scales they include depressed temperature and helium abundance and elevated density, charge-state ratios, and elemental abundance ratios. At medium scales these parameters are highly variable. At small scales the magnetic field magnitude plays a major role in defining structures with high plasma beta and isotropic suprathermal electron distributions. Other slow wind properties of interest include evidence for a boundary layer and the relationship of slow wind structures to the heliospheric current sheet (HCS). Against expectations, a relatively large fraction of spacecraft passages through the slow wind lack HCS crossings. Seen as a whole, the observed properties of the slow wind suggest a synthesis view with both steady-state and transient aspects.

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