{'fraction_non_alphanumeric': 0.020585048754062838, 'fraction_numerical': 0.0, 'mean_word_length': 5.201342281879195, '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}}
INFLUENCE OF NON-THERMAL PROCESSES ON LINE ASYMMETRIES IN SOLAR FLARES

We make line profile calculations for a flare atmosphere considering simultaneously the effect of non-thermal excitation and ionization of the hydrogen atoms caused by precipitating high-energy electrons, and the effect of possible chromospheric downflows. The results confirm the earlier finding that a downflow, if confined to the upper chromosphere, can sometimes produce a blue asymmetry of the Hα line. In addition, we find that the existence of such non-thermal effects tends to enhance the blue-asymmetry magnitude. In particular, the larger the energy flux, or the harder the energy spectrum for the beam electrons, the easier it will be to produce a blue-asymmetric Hα profile, which is simultaneously intensified and broadened. Possible reasons which make the blue asymmetry less popular than the red asymmetry in observations are discussed.