{'fraction_non_alphanumeric': 0.01699346405228758, 'fraction_numerical': 0.022222222222222223, 'mean_word_length': 4.550724637681159, '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}}
An Ionized Accretion Flow in the Ultracompact H II Region G10.6–0.4

Analysis of the H66α radio recombination line velocities in the ultracompact H II region G10.6-0.4 indicates inward motion of the ionized gas within the H II region. Comparison with the velocities of molecular lines from the surrounding neutral gas suggests that a molecular accretion flow passes through the ionization boundary of the H II region and continues inward as an ionized accretion flow. Interpreted in the context of a model for star formation in hot molecular cores, these observations indicate that G10.6-0.4 is at a stage of development just after the massive star or stars at the center of the accretion flow have first formed an ionized H II region within the hot molecular core.