Feb. 25, 2005
Bldg 21, Rm 183, 12:00 noon

Acceleration Region of the Solar Wind
Leon Ofman
CUA, NASA/GSFC

The acceleration of the fast solar wind takes place within 10 Rs, and coronal holes have been
identified as the source regions of the fast solar wind. MHD wave activity has been detected in
coronal holes by remote sensing, and in-situ in fast solar wind streams. I will review some of the
most suggestive wave observations, and discuss the theoretical aspects of MHD wave heating and solar
wind acceleration in coronal holes. I will present the results of single fluid 2.5D MHD, as well as
multi-fluid 2.5D MHD models of solar wind acceleration regions, and discuss some of the likely
heating, and the acceleration mechanisms. I will discuss future observations in the acceleration
region of the solar wind proposed for the Solar Probe mission, currently being studied by NASA.