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Three of the most important and most puzzling features of the Sun'satmosphere are the smoothness of the closed field corona, the accumulation ofmagnetic shear at photospheric polarity inversion lines (PIL), and thecomplexity of the slow wind. We propose that a single process, helicitycondensation, is the physical mechanism giving rise to all three features. Asimplified model is presented for how helicity is injected and transported inthe closed corona by magnetic reconnection. With this model we demonstrate thathelicity must condense onto PILs and coronal hole boundaries, and estimate therate of helicity accumulation at PILs and the loss to the wind. Our results canaccount for many of the observed properties of the closed corona and wind.

Helicity Condensation as the Origin of Coronal and Solar Wind Structure