{'fraction_non_alphanumeric': 0.017064846416382253, 'fraction_numerical': 0.010238907849829351, 'mean_word_length': 4.983673469387755, 'pattern_counts': {'":': 0, '<': 0, '<?xml version=': 0, '>': 0, 'https://': 0, 'lorem ipsum': 0, 'www.': 0, 'xml': 0}, 'pii_count': 0, 'substrings_counts': 0, 'word_list_counts': {'cursed_substrings.json': 0, 'profanity_word_list.json': 0, 'sexual_word_list.json': 0, 'zh_pornsignals.json': 0}}
Observations of Separator Reconnection to an Emerging Active Region

Extreme-ultraviolet (EUV) observations of an emerging active region are used to study separator reconnection in the corona. We identify each EUV loop connecting the emerging polarity to a nearby existing active region over the 41 hr period beginning at emergence onset. Their geometrical resemblance to post-reconnection field lines from a magnetic model of the active region pair implicates separator reconnection in their production. While some reconnection is evident within 7 hr of emergence onset, the most intense period occurs after a 1 day delay. The sum of cross sections of all observed loops accounts for only one-fifth of the transferred magnetic flux predicted by the model. We suggest that the remaining loops remain at temperatures too high, or at densities too low, to be detected in our EUV data. The most intense reconnection requires as much as 109 V along the coronal separator; however, the observed loops suggests that the flux is transferred as discrete bundles of ~4 × 1018 Mx each. The reconnection appears to directly dissipate only a small fraction of the energy released, while the rest is dissipated within the post-reconnection flux over the ensuing 6 or more hours the loops remain visible. The net energy released, and ultimately dissipated, is consistent with the amount that could be stored magnetically during the 24 hr delay between emergence and reconnection.