Transforming a Turbulent Corona into a Turbulent Wind

Solar Wind 9 , 1998

R. Grappin, J. Léorat

Abstract

We illustrate the possibility that the accelerating region of the solar wind is the birthplace of both jet-like phenomena and of the quasi-incompressible turbulence observed in situ at largest distances. We consider axisymetric, time-dependent isothermal MHD simulations in a shell containing the sonic point, within an external dipolar magnetic field, with beta about unity or larger. We use as boundary conditions an ad hoc model of turbulent corona which leads to a) the quasi-periodic ejection of compressive blobs in the current sheet region b) an eddy circulation advected by the wind.
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