  Three of the most important and most puzzling features of the Sun's
atmosphere are the smoothness of the closed field corona, the accumulation of
magnetic shear at photospheric polarity inversion lines (PIL), and the
complexity of the slow wind. We propose that a single process, helicity
condensation, is the physical mechanism giving rise to all three features. A
simplified model is presented for how helicity is injected and transported in
the closed corona by magnetic reconnection. With this model we demonstrate that
helicity must condense onto PILs and coronal hole boundaries, and estimate the
rate of helicity accumulation at PILs and the loss to the wind. Our results can
account for many of the observed properties of the closed corona and wind.
