3:30 PM - 4:50 PM
The origin of the slow solar wind is controversial. One group of theories argues that the slow wind primarily arises quasi-statically from the large magnetic expansion factor in these regions, while another set of theories contends that a significant portion of the slow solar wind arises dynamically via the reconnection of open and closed fields in the corona. In this talk, I describe modeling results that show that the dynamic interaction between open and closed fields is closely related to the evolution of coronal holes. Observations of coronal holes in the STEREO era may thus prove to be important discriminator between the different theories.