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Session 74 - The Quiet & Active Sun.
Display session, Friday, January 09
Exhibit Hall,
We use the 2.5D (3D with azimuthal symmetry) MHD equations to
model numerically the solar wind acceleration in a
nonhomogeneous coronal hole. We investigate the parametric
dependence of the solar wind acceleration by nonlinear MHD
waves with a monochromatic and a broad band driving source. We
find that when the Alfvèn wave amplitude is above a
parameter dependent threshold , large amplitude nonlinear
longitudinal waves are generated and contribute to the radial
acceleration. The calculated solar wind speed and density
fluctuates considerably on a time scale of tens of minutes
with an amplitude of up to several hundred km/s near the sun
(4R_ødot
The author(s) of this abstract have provided an email address for comments about the abstract: Leon.Ofman@gsfc.nasa.gov
