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

Abstract

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 16.87177 ± 0.02084 days and a long period of 587 days. 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 ∆V= 0.1 mag. Assuming synchronous rotation for the cool stellar component and semi-detached 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% 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%, fit the light curve asymmetries. The system is seen under inclination 67.4 ± 0.4 degree 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 anti-phase 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.

New insights on the massive interacting binary UU Cassiopeiae

“…The temperature of the disk matches the temperature of the gainer on its inner edge and decreases with a radial profile described by an exponent a T . The model has been described in several papers, such as Mennickent & Djurašević (2013), Mennickent et al (2015), Mennickent (2019), where more details can be found.…”

Doppler tomography of the Double periodic variable HD 170582 at low and high stage

“…The stellar parameters used in this paper to find the best evolutionary model for HD 170582. Data are from Mennickent et al (2015). quantity value quantity value…”

“…It was recently studied by Mennickent et al (2015), who found a slightly evolved B-type star surrounded by a luminous accretion disc fed by a Roche-lobe overflowing Atype giant. Here we extend their analysis presenting new spectroscopic data and studying the Balmer emission lines.…”

Orbital and superorbital periods in ULX pulsars, disc-fed HMXBs, Be/X-ray binaries, and double-periodic variables

“…These DPV stars have also been observed as spectroscopic binaries (e.g. Mennickent et al 2005;Mennickent et al 2012;Mennickent et al 2015;Barría et al 2014), showing that they consist of an early B-type main sequence star and a hot, lower-mass, but evolved companion (i.e. an Algol-like system).…”

“…Finally, the mechanism producing the longer period in the DPV systems is also found in BeXRBs. Mennickent et al (2015) show a schematic of a DPV depicting the locations of a hot spot and bright spot on the Be star disc. The precession of the bright spot on the disc is equivalent to the precession of a density wave that produces the super-orbital periods in BeXRBs.…”