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Accurate forecasting of space weather requires knowledge of the sourceregions where solar energetic particles (SEP) and eruptive events originate.Recent work has linked several major SEP events in 2014, January, to specificfeatures in the host active region (AR 11944). In particular, plasmacomposition measurements in and around the footpoints of hot, coronal loops inthe core of the active region were able to explain the values later measuredin-situ by the Wind spacecraft. Due to important differences in elementalcomposition between SEPs and the solar wind, the magnitude of the Si/Selemental abundance ratio emerged as a key diagnostic of SEP seed populationand solar wind source locations. We seek to understand if the results aretypical of other active regions, even if they are not solar wind sources or SEPproductive. In this paper, we use a novel composition analysis technique,together with an evolutionary magnetic field model, in a new approach toinvestigate a typical solar active region (AR 11150), and identify thelocations of highly fractionated (high Si/S abundance ratio) plasma. Materialconfined near the footpoints of coronal loops, as in AR 11944, that in thiscase have expanded to the AR periphery, show the signature, and can be releasedfrom magnetic field opened by reconnection at the AR boundary. Since thefundamental characteristics of closed field loops being opened at the ARboundary is typical of active regions, this process is likely to be general.

Signature and escape of highly fractionated plasma in an active region