The evolution stage and massive disc of the interacting binary V 393 Scorpii

Abstract

V 393 Scorpii is a bright Galactic Double Periodic Variable showing a long photometric cycle of ≈253 d. We present new VIJK photometric time series for V 393 Scorpii along with the analysis of All Sky Automated Survey (ASAS) V-band photometry. We disentangled all light curves into the orbital and long-cycle components. The ASAS V-band orbital light curve was modelled with two stellar components plus a circumprimary optically thick disc assuming a semi-detached configuration. We present the results of this calculation, giving physical parameters for the stars and the disc, along with general system dimensions. Our results are in close agreement with those previously found by Mennickent et al. from infrared (IR) spectroscopy and the modelling of the spectral energy distribution. The stability of the orbital light curve suggests that the stellar plus disc configuration remains stable during the long cycle. Therefore, the long cycle should be produced by an additional variable and not-eclipsed emitting structure. We discuss the evolutionary stage of the system finding the best match with one of the evolutionary models of van Rensbergen et al. According to these models, the system is found to be after an episode of fast mass exchange that transferred 4 M from the donor to the gainer in a period of 400 000 years. We argue that a significant fraction of this mass has not been accreted by the gainer but remains in an optically thick massive (∼2 M ) disc-like surrounding pseudo-photosphere whose luminosity is not driven by viscosity but probably by reprocessed stellar radiation. Finally, we provide the result of our search for Galactic Double Periodic Variables and briefly discuss the outliers β Lyr and RX Cas.

Fundamental stellar and accretion disc parameters of the eclipsing binary DQ Velorum

“…We separated multiperiodic V, I, J, and K light curves with a Fourier decomposition technique (for more details see Demircan 1979;Mennickent et al 2012a) and found two main Fourier components of frequencies f 1 and f 2 , the sum of which (including their most important harmonics) is the best representation of the light curves. f 1 is higher and associated with a period of 6.083299 d, which represents the orbital variability of the binary (see Fig.…”

“…At present, there are more than 150 DPVs discovered in the Magellanic Clouds and 11 systems (including DQ Vel) in the Milky Way (Mennickent et al 2012a). Results of multiwavelength spectroscopy and/or photometry have made it possible to study DPVs in more detail, such as AU Mon (Desmet et al 2010;Djurašević et al 2010), V393 Sco (Mennickent et al , 2012a, and LP Ara (Mennickent et al 2011).…”

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

“…We find that HD 170882 shows spectroscopic properties similar to other DPVs like AU Monocerotis, V 393 Scorpii, DQ Velorum and OGLE 05155332-6925581 (Mennickent et al, 2008, 2012a, 2012b, Barría et al 2013, Garrido et al 2013. These properties include the existence of an optically thick disc surrounding a B-type star and evidence for stream-disc interaction.…”

“…We noticed that the ASAS period (16.8599 days) does not fit the periodogram minimum as well as our period, probably because of the automatic character of the period searching algorithm used in this catalogue and the lack of filtering of bad data points. The light curve was disentangled with these two periods using the software written by Zbigniew Kołaczkowski and described in Mennickent et al (2012a). Afterwards, the resulting disentangled light curves were folded with both periods as shown in Fig.…”

“…It is located in the region of the cool molecular cloud L 379 and was observed by Lahulla and Hilton (1992) who obtained V = 9.62 mag, B−V = 0.44 mag and U − B = -0.27 mag. The system is characterized by a long photometric cycle of 536 days and is the third longest-period member of the Galactic Double Period Variables (DPVs), after V 495 Cen and V 4142 Sgr (Mennickent & Rosales 2014, Mennickent et al 2012a. DPVs are intermediate mass interacting binaries showing a long photometric cycle lasting about 33 times the orbital pe-riod, which has been interpreted as cyclic episodes of mass loss (Mennickent et al 2003, Mennickent et al 2008, 2012b, Poleski et al 2010).…”