{'fraction_non_alphanumeric': 0.02387774594078319, 'fraction_numerical': 0.02387774594078319, 'mean_word_length': 4.634408602150538, '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}}
Periodic Variability in the Pre-Main-Sequence Object CB 34V

A photometric study of the G-type pre–main-sequence star CB 34V was undertaken at Van Vleck Observatory during the 2001–2002 observing season. The star remained in its bright state throughout the 5 month monitoring period, showing no evidence of the large amplitude variability that originally drew attention to it. However, it did exhibit periodic variability with an amplitude of ∼0.6 mag. A highly significant peak is present in the periodogram at 1.186 days, but analysis of the light curve suggests that the actual rotation period of the star is twice that—2.372 days. Apparently, the star had similar spots on opposite hemispheres during this time and we view it close to equator-on. This circumstance allows us to place additional constraints on the radius and luminosity of the star. The new data argue against its being an FU Orionis star and in favor of its being either a UX Orionis star or an object (similar to KH 15D) that is eclipsed episodically by circumstellar matter.