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We explore the use of observed polar coronal holes (CHs) to constrain theflux distribution within the polar regions of global solar magnetic field mapsin the absence of reliable quality polar field observations. Global magneticmaps, generated by the Air Force Data Assimilative Photospheric flux Transport(ADAPT) model, are modified to enforce field unipolarity thresholds both withinand outside observed CH boundaries. The polar modified and unmodified maps areused to drive Wang-Sheeley-Arge (WSA) models of the corona and solar wind (SW).The WSA predicted CHs are compared with the observations, and SW predictions atthe WIND and Ulysses spacecraft are also used to provide context for the newpolar modified maps. We find that modifications of the polar flux never worsenand typically improve both the CH and SW predictions. We also confirm theimportance of the choice of the domain over which WSA generates the coronalmagnetic field solution but find that solutions optimized for one location inthe heliosphere can worsen predictions at other locations. Finally, weinvestigate the importance of low-latitude (i.e., active region) magneticfields in setting the boundary of polar CHs, determining that they have atleast as much impact as the polar fields themselves.

Solar Polar Flux Redistribution based on Observed Coronal Holes