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We aim to characterize the stellar wind, constrain the system geometry, and investigate the origin and variability of the Fe K$\\alpha$ fluorescence line.\n  Methods. We analyzed three Chandra HETGS observations at different orbital phases. The continuum was modeled with a bulk motion Comptonization (Bmc) model including partial-covering absorption. We performed a blind line search with Monte Carlo simulations accounting for the look-elsewhere effect. 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