http://arxiv.org/abs/1811.02349
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 when the source came back to quiescence. The object was detected as a weak X-ray source ($0.01103\pm0.0014$ counts s$^{-1}$) in the plateau of the superoutburst and its flux dropped sharply at the end of the fading stage ($0.0006\pm0.0005$ counts s$^{-1}$). An extended emission around the source was observed up to 30 days after the peak of the superoutburst, interpreted it as a bow-shock formed by a wind from the source. The head of the bow-shock is coinciding with the high-proper motion vector of the source ($v_{\perp}=123\pm5$ km s$^{-1}$) at a distance of $d=202\pm7$ pc. From spectroscopic observations in quiescence we confirmed the orbital period value $P_{\rm{orb}}=0.0545\pm 0.0026$ days, consistent with early-superhump estimates, and the following orbital parameters: $\gamma= -21\pm3$ km s$^{-1}$ and $K_1 = 53\pm3$ km s$^{-1}$. The white dwarf is revealed when the system approaches quiescence, which enables us to infer the effective temperature of the primary $T_{eff}=11,600\pm400$K. The donor temperature of V1838 Aql is estimated to be $\lesssim 2200$K and suggestive of a system approaching the period minimum. Doppler maps of the system in quiescence show the presence of the bright hot spot in HeI line at the expected accretion disc-stream shock position and an unusual structure of the accretion disc in H$\alpha$.
J. Santisteban, J. Echevarría, S. Zharikov, et. al.
Wed, 7 Nov 18
84/94
Comments: 14 pages, 8 figures, submitted to MNRAS. Comments are welcome
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