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. (2019-04-08)
J V Hernández Santisteban, J Echevarría, S Zharikov, V Neustroev, G Tovmassian, V Chavushyan, R Napiwotzki, R Costero, R Michel, L J Sánchez, A Ruelas-Mayorga, L Olguín, Ma T García-Díaz, D González-Buitrago, E de Miguel, E de la Fuente, R de Anda, V Suleimanov, From outburst to quiescence: spectroscopic evolution of V1838 Aql imbedded in a bow-shock nebula, Monthly Notices of the Royal Astronomical Society, Volume 486, Issue 2, June 2019, Pages 2631–2642, https://doi.org/10.1093/mnras/stz798
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. © 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
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https://urn.fi/URN:NBN:fi-fe2019090426588
Tiivistelmä
Abstract
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.
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