Investigations of a turbulence-driven solar wind model

Details Investigations of a turbulence-driven solar wind model Investigations of a turbulence-driven solar wind model

May 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990jgr....95.6437i&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 95, May 1, 1990, p. 6437-6442.

Physics

62

Kolmogoroff Theory, Magnetohydrodynamic Waves, Solar Physics, Solar Wind, Turbulence Effects, Two Fluid Models, Electron Energy, Proton Energy, Spatial Distribution, Supersonic Flow, Transonic Flow, Turbulent Heat Transfer

Scientific paper

This work presents an investigation of the properties of the one-dimensional, two-fluid turbulence-driven solar wind model introduced by Hollweg and Johnson (1988). It is found that the model has serious difficulties in reproducing the observed high-speed wind at 1 AU. In particular, the model proton temperatures are lower than those observed by a factor of 2 or more, and the highest temperature models yield excessive wave intensities at 1 AU. It appears that the problem stems from the specific spatial distribution of heat deposition in the model. Thus this study does not rule out a turbulence-driven fast solar wind, since other forms of the turbulent evolution could probably achieve better results. A three-fluid version of the model is also presented to show that the addition of alpha particles does not significantly reduce the extreme proton temperatures displayed near the sun by the Hollweg and Johnson work. Finally, it is suggested that the additional heating needs to be located well beyond the critical point, implying that the heating mechanism for the fast solar wind is likely not the same as that heating the solar corona.

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