The Large-Scale Variability of Solar Wind Streams

Details The Large-Scale Variability of Solar Wind Streams The Large-Scale Variability of Solar Wind Streams

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh32a0729r&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH32A-0729

Physics

2102 Corotating Streams, 2134 Interplanetary Magnetic Fields, 2162 Solar Cycle Variations (7536), 2164 Solar Wind Plasma, 2169 Sources Of The Solar Wind

Scientific paper

Fast and slow solar wind are fundamentally different. In particular, slow solar wind shows a significant and persistent variability that is absent in the fast wind. It is generally believed that this structure is driven by a combination of temporal and spatial variations, however, its origin remains poorly understood. It has been suggested, for example, that the super-radial expansion of magnetic field lines near the Sun governs the speed (and hence variability) of the solar wind. Alternatively (or in addition to), it has been proposed that the combination of differential rotation of the photosphere, together with non-radial expansion of the solar wind through approximately rigidly-rotating coronal holes leads to the opening of formerly closed magnetic structures thereby releasing plasma into the solar wind. In the first mechanism, the variability of the slow solar wind is predominantly due to spatial variations in the solar magnetic field, whereas in the second mechanism, the process is sporadic and dynamically driven. In this study we use a combination of 3-D, time-dependent MHD simulations, remote solar measurements, and in situ observations to explore the contribution of temporal and spatial variability to the overall large-scale structure of the solar wind from the solar surface to 5 AU.

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