{'fraction_non_alphanumeric': 0.03454715219421102, 'fraction_numerical': 0.06069094304388422, 'mean_word_length': 4.153846153846154, '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}}
ECLIPSING BINARIES WITH NODAL MOTION - ARCHIVAL DATA

This paper presents a study of the three eclipsing binaries IU Aur, NQ Her, and AY Mus for times before 1943. The data were obtained from examination of archival photographic plates in the collection of Harvard College Observatory. IU Aur was found to have an amplitude of 0m.18 ± 0m.05 in 1890-04 and 0m.24 ± 0m.04 in 1931-36. These amplitudes are used to derive an inclination of the eclipsing binary's orbital plane of 61° ± 2° and 66° ± 2°, respectively. A nodal rotation period of 150 years is most likely. The angle between the orbital planes of the eclipsing binary and the third body is 15°.8. The previous reported period of NQ Her, 0d.870218, is shown to be erroneous, so that previous claims of nodal motion in this system are unfounded. AY Mus was found to be eclipsing with a period of 3d.20559 for the years 1897 to 1943. This confirmation of the eclipsing nature, when combined with a 1973 observation that AY Mus no longer eclipses, suggests that nodal motion is the cause for the stoppage of eclipse.