The drivers of active region outflows into the slow solar wind

Hinode/EIS observations show large areas of Doppler blue-shifted outflows at the edges of active regions, and these have been suggested as a possible source of the slow solar wind. The outflows appear more spatially extended at higher temperatures (~2MK), but views of the base at lower temperatures are often obscured by bright fan loops dominated by downflows. At the spatial resolution of EIS, it has therefore been difficult to clearly determine what is driving the outflows. The High-resolution Coronal Imager (Hi-C) flew on a sounding rocket in May 2018, and observed areas of active region outflow at the highest spatial resolution ever achieved in the EUV. EIS spectral line intensity measurements were obtained in coordination with the Hi-C flight, and we used them to compute the elemental composition in the outflows. We then used the high spatial resolution intensity images from Hi-C to try to understand what features are contributing to the intensities detected by EIS at lower spatial resolution, and therefore determine what structures dominate the EIS composition signature. We will report the results of this analysis.