How are properties of superhalo electrons and SEPs differentiated by their solar source regions?

In previous studies we have found that elemental composition in gradual SEP events is governed, at least in part, by the strength of the photospheric magnetic field around the footpoints of the IMF along which the SEPs are transported. The SEP elemental composition differs depending on whether the solar footpoint of the IMF is in a ';quiet' coronal hole (without a nearby active region) or in an ';active' coronal hole (with a nearby active region). These studies suggest that magnetic reconnection in footpoint regions near active regions bias the heavy-ion composition of suprathermal seed ions by processes qualitatively similar to those that produce larger heavy-ion enhancements in impulsive SEP events. In this study, we further investigate this aspect by looking for correlations among the properties in a large sample of regions in the close vicinity of coronal holes (i.e. open field regions), such as the photospheric magnetic field and flare rate, and the correlations between these properties and those in the associated superhalo electrons measured in-situ during non-event periods and in the associated gradual SEP events during event periods.