{"paper":{"title":"1RXS J174320.1-042953: another polar with a red-shifted absorption component in emission line wings","arxiv_id":"2610.01032","primary_cat":"astro-ph.SR","submitted_at":"2026-10-01T04:19:01+00:00","version_compiled":"v1"},"notice":"Every quoted sentence is the authors' text from the arXiv listing abstract. Labels and probabilities are the outputs of classifier-1.13.0 on the question bank abstract-p1-20260923, exactly as returned. No sentence in this record was written by a language model.","schema":"pith.compiled-record/v0","status":"compiled","abstract":{"source":"arXiv listing abstract v1","sentences":[{"i":0,"p":1.0,"id":"s0","own":true,"role":"contribution","text":"We present the results of a spectroscopic and multi-band photometric study of the magnetic cataclysmic variable 1RXS J174320.1-042953.","hedge":{"p":0.94,"label":"asserted"},"own_p":0.89,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.13,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":1.0,"interpretation":0.0}},{"i":1,"p":1.0,"id":"s1","own":true,"role":"result","text":"Multi-band photometry confirms a periodic modulation with an orbital period of $P_{\\rm orb}=0.0864 \\pm 0.0001$ days.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.88,"main_claim_p":0.06,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":2,"p":1.0,"id":"s2","own":true,"role":"result","text":"Using the estimated secondary mass of $\\sim0.15\\,\\mathrm{M_\\odot}$ and, the X-ray-based white dwarf mass of $\\sim0.75\\,\\mathrm{M_\\odot}$, we obtain values of $q\\sim0.2$ and a system inclination of $47^\\circ\\pm10^\\circ$.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.93,"main_claim_p":0.06,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":3,"p":0.97,"id":"s3","own":true,"role":"result","text":"The optical spectra of 1RXS J174320.1-042953 are dominated by strong, complex, asymmetric, and highly variable single-peaked emission lines of the Balmer series, \\ion{He}{i}, and \\ion{He}{ii}, which are characteristic of polar-type magnetic cataclysmic variables.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.88,"main_claim_p":0.13,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.97,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.02}},{"i":4,"p":0.82,"id":"s4","own":true,"role":"result","text":"Doppler tomography reveals no evidence of a Keplerian accretion disc, supporting the classification of the system as a polar.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.94,"main_claim_p":0.16,"quantitative":false,"quantitative_p":0.09,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.82,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.01,"interpretation":0.16}},{"i":5,"p":1.0,"id":"s5","own":true,"role":"result","text":"The H$\\beta$ and \\ion{He}{ii} emission lines can be decomposed into at least two distinct components.","hedge":{"p":0.9,"label":"asserted"},"own_p":0.9,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.5,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"The low-velocity components have semi-amplitudes of approximately 170 km s$^{-1}$ (H$\\beta$) and 147 km s$^{-1}$ (\\ion{He}{ii}), while the high-velocity components reach about 317 km s$^{-1}$ and 460 km s$^{-1}$, respectively.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.93,"main_claim_p":0.05,"quantitative":true,"quantitative_p":0.99,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":7,"p":1.0,"id":"s7","own":true,"role":"interpretation","text":"The low-velocity component is likely associated with the irradiated side of the secondary star facing the white dwarf and/or the vicinity of the L$_1$ point, whereas the high-velocity component is related to the accretion-stream structure.","hedge":{"p":0.99,"label":"hedged_possibility"},"own_p":0.74,"main_claim_p":0.08,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":1.0}},{"i":8,"p":0.94,"id":"s8","own":true,"role":"result","text":"A redshifted absorption component in the emission-line wings is detected at orbital phases near $\\phi \\approx 0.0$, reaching velocities up to $\\sim1400$ km s$^{-1}$ and likely produced by accretion-stream material crossing the line of 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