From outburst to quiescence: spectroscopic evolution of V1838 Aql imbedded in a bow-shock nebula

Hernández Santisteban, J. V.; Echevarría, J.; Zharikov, S.; Neustroev, V.; Tovmassian, G.; Chavushyan, V.; Napiwotzki, R.; Costero, R.; Michel, R.; Sánchez, L. J.; Ruelas-Mayorga, A.; Olguín, L.; García-Díaz, Ma. T.; González-Buitrago, D.; de Miguel, E.; de la Fuente, E.; de Anda, R.; Suleimanov, V.
Monthly Notices of the Royal Astronomical Society, Volume 486, Issue 2, p.2631-2642 (2019).


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 Porb = 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 Teff = 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.