{'fraction_non_alphanumeric': 0.030166880616174584, 'fraction_numerical': 0.03337612323491656, 'mean_word_length': 4.817164179104478, '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}}
Unraveling the Puzzle of the Eclipsing Polar SDSS J015543.40+002807.2 with XMM and Optical Photometry/Spectropolarimetry

The cataclysmic variable SDSS J015543.40+002807.2 is confirmed to be a magnetic system of the AM Herculis type. With an orbital period of 87.13 minutes, it is also the shortest period eclipsing Polar known. Monitoring with XMM-Newton finds a high-state light curve dominated by a single X-ray-emitting accretion pole located slightly prograde of the secondary star. The hard X-ray spectrum is typical of radial shocks on magnetic white dwarfs (kT ~ 10 keV), and there is evidence for a soft X-ray component consistent with reprocessing from the stellar surface. The optical circular polarization is weak (v ≲ 3%) when the accretion rate is high (mV ~ 15.5), as a result of optically thick cyclotron emission and the apparent competition between two accreting poles. However, in low states (mV ~ 18), the polarization increases smoothly to the blue, reaching 20% at 4200 Å, and the flux spectrum displays a rich set of thermally broadened cyclotron harmonics that indicate a polar field of 29 MG. The phase interval preceding the 6.5 minute eclipse depicts the development of P Cygni components followed by complete absorption reversals in the emission lines. This phenomenon is not unexpected for a strongly accreting magnetic system viewed through the cool base of the funnel, and high-quality spectroscopy through this interval will likely lead to new insights into the dynamics of magnetic coupling and gas flow onto the white dwarf.