2019MNRAS.486.2631H

We analyse new optical spectroscopic, direct-image and X-ray observations of the recently discovered a high-proper motion cataclysmic variable V1838 Aql. The data were obtained during its 2013 superoutburst and its subsequent quiescent state. An extended emission around the source was observed up to 30 d after the peak of the superoutburst, interpreted it as a bow shock formed by a quasi-continuous outflow from the source in quiescence. The head of the bow shock is coincident with the high-proper motion vector of the source (v_⊥ = 123 ± 5 km s^–1) at a distance of d = 202 ± 7 pc. The object was detected as a weak X-ray source (0.015 ± 0.002 counts s^–1) in the plateau of the superoutburst and its flux lowered by two times in quiescence (0.007 ± 0.002 counts s^–1). Spectroscopic observations in quiescence we confirmed the orbital period value P_orb = 0.0545 ± 0.0026 d, consistent with early-superhump estimates, and the following orbital parameters: γ = -21 ± 3 km s^–1 and K₁ = 53 ± 3 km s^–1. The white dwarf is revealed as the system approaches quiescence, which enables us to infer the effective temperature of the primary T_eff = 11 600 ± 400 K. The donor temperature is estimated <=2200 K and suggestive of a system approaching the period minimum. Doppler maps in quiescence show the presence of the hotspot in He I line at the expected accretion disc-stream shock position and an unusual structure of the accretion disc in Hα.