Active Region Contributions to the Solar Wind over Multiple Solar Cycles

Both coronal holes and active regions are source of the solar wind. The distribution these structures across both space time is well known, but it unclear how much each contributes to In this study we use photospheric magnetic field maps observed over past four cycles estimate what fraction open flux rooted in regions, a proxy for all wind originating regions. We find that fractional contribution varies between 30% 80% at any one during maximum negligible minimum, showing strong correlation with sunspot number. While typically confined latitudes $\pm$30$^{\circ}$ corona, they produce can reach up $\pm$60$^{\circ}$. Their also correlates mass ejection rate, highly variable, changing by $\pm$20% on monthly timescales within individual maxima. speculate variations could be driven ejections causing reconfigurations sub-monthly timescales.