Computer Science
Scientific paper
Jun 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aipc..471..155m&link_type=abstract
The solar wind nine conference. AIP Conference Proceedings, Volume 471, pp. 155-160 (1999).
Computer Science
1
Magnetohydrodynamics And Plasmas, Solar Wind Plasma, Sources Of Solar Wind
Scientific paper
The solar wind low-frequency turbulence is characterized by fluctuations which are mainly Alfvénic, with high cross-helicity and low-amplitude compressive fluctuations. These features are locally lost, in the presence of strong inhomogeneities of the background medium, like velocity shears due to the stream structure, current sheets at magnetic sector boundaries, large-scale density and temperature inhomogeneities. Such nonuniformities generate a coupling among different modes and tend to destroy the equilibrium solution represented by outward propagating Alfvénic fluctuations. The Alfvénicity is also reduced with increasing distance from the Sun, and this could be in part due to the effects of the large-scale inhomogeneity related to the solar wind expansion. The effects of inhomogeneities of the background medium on a MHD turbulence have been studied, from a theoretical point of view, by a number of numerical models. In this paper we briefly review such models, discussing the main results and their limitations, and comparing with observed features of the solar wind fluctuations.
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