Fundamental parameters of the close interacting binary HD 170582 and its luminous accretion disc

• Published in: Monthly notices of the Royal Astronomical Society 2015-04, Vol.448 (2), p.1137-1152
• Main Authors: Mennickent, R. E., Djurašević, G., Cabezas, M., Cséki, A., Rosales, J. G., Niemczura, E., Araya, I., Curé, M.
• Format: Article
• Language: English
• Subjects: Accretion disks; Astronomy; Asymmetry; Dwarf stars; Ephemerides; Inclination; Light curve; Luminosity; Orbitals; Photometry; Radial velocity; Star & galaxy formation; Stars
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stv008

We present a spectroscopic and photometric study of the double period variable HD 170582. Based on the study of the ASAS V-band light curve, we determine an improved orbital period of 16.871 77 ± 0.020 84 d and a long period of 587 d. We disentangled the light curve into an orbital part, determining ephemerides and revealing orbital ellipsoidal variability with unequal maxima, and a long cycle, showing quasi-sinusoidal changes with amplitude ΔV= 0.1 mag. Assuming synchronous rotation for the cool stellar component and semidetached configuration we find a cool evolved star of M 2 = 1.9 ± 0.1 M⊙, T 2 = 8000 ± 100 K and R 2 = 15.6 ± 0.2 R⊙, and an early B-type dwarf of M 1 = 9.0 ± 0.2 M⊙. The B-type star is surrounded by a geometrically and optically thick accretion disc of radial extension 20.8 ± 0.3 R⊙ contributing about 35 per cent to the system luminosity at the V band. Two extended regions located at opposite sides of the disc rim, and hotter than the disc by 67 and 46 per cent, fit the light-curve asymmetries. The system is seen under inclination 67 $_{.}^{\circ}$ 4 ± 0 $_{.}^{\circ}$ 4 and it is found at a distance of 238 ± 10 pc. Specially interesting is the double line nature of He i 5875; two absorption components move in antiphase during the orbital cycle; they can be associated with the shock regions revealed by the photometry. The radial velocity of one of the He i 5875 components closely follows the donor radial velocity, suggesting that the line is formed in a wind emerging near the stream–disc interacting region.