{'fraction_non_alphanumeric': 0.02306805074971165, 'fraction_numerical': 0.02883506343713956, 'mean_word_length': 4.228915662650603, '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}}
LAMBDA PERSEI: AN UNUSUAL B9 IV STAR

Spectrograms of Lambda Per obtained at 30 A/mm in the red region show weak emission peaks in the core of the H-alpha absorption line. The V/R for the emission components changed from about 1.0 on October 28 1990 UT to less than 1.0 on October 29, 1990 UT. The midpoints of absorption lines from He I, Si II, Fe II, and the midpoints of the H-alpha profile measured at residual intensities between 0.80 and 0.96 are shifted slightly shortward of the wavelengths suggested by the catalog radial velocities of Lambda Per and by the wavelength of the sharp central absorption core of H-alpha. It is plausible that the emission features originate in plage areas on the surface of Lambda Per, and that the aspect of the plages presented to the observer changes as the star rotates. Plages imply the presence of surface magnetic fields.