Investigating the Possible Contribution of Helicity Condensation to the Ambient Increase in Solar Open Flux

Abstract The Sun’s Open Flux plays a vital role in heliospheric physics and for the origin of the solar wind. A key problem faced by global magnetic field models of the solar corona is that they consistently underestimate the amount of Open Flux compared to in situ measurements. The purpose of the present paper is to consider if statistically averaged helicity condensation (SAHC) can reduce this discrepancy by increasing the simulated Open Flux found in potential field source surface (PFSS) models. We consider each Carrington rotation from 1646–2149 (1976 September to 2014 April). For each rotation, we hold the photosphere fixed, construct a PFSS model, and inject nonpotentiality into the coronal field by applying SAHC at different angular rotation rates, ω . When ω exceeds 2.5 × 10 −6 s −1 , both ambient and sporadic enhancements of Open Flux are found within the Carrington rotation timescale. As ω increases, the amount of ambient Open Flux increases, along with the frequency of sporadic events. These enhancements are accompanied by increased footpoint area of open field lines, where the open field locations at each pole expand by up to 3 ∘ –6 ∘ of latitude. A solar cycle dependence is found with higher increases in ambient Open Flux at solar maximum compared to solar minimum. Comparing our results with 27 day averaged OMNI spacecraft measurements, our highest value of ω = 10 × 10 −6 s −1 can resolve just under 50% of the discrepancy between in situ Open Flux measurements and PFSS models. Although helicity condensation cannot fully resolve the discrepancy, it can significantly contribute toward reducing it.