Accretion disc in the eclipsing binary AU Mon★

Djurašević, G.; Latković, O.; Vince, I.; Cséki, A.

doi:10.1111/j.1365-2966.2010.17310.x

Cited by 23 publications

(30 citation statements)

References 32 publications

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“…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).…”

Section: Introductionmentioning

confidence: 99%

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

Barría

Mennickent

Schmidtobreick

et al. 2013

A&A

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Context. To add to the growing collection of well-studied double periodic variables (DPVs) we have carried out the first spectroscopic and photometric analysis of the eclipsing binary DQ Velorum to obtain its main physical stellar and orbital parameters. Aims. Combining spectroscopic and photometric observations that cover several orbital cycles allows us to estimate the stellar properties of the binary components and the orbital parameters. We also searched for circumstellar material around the more massive star. Methods. We separated DQ Velorum composite spectra and measured radial velocities with an iterative method for double spectroscopic binaries. We obtained the radial velocity curves and calculated the spectroscopic mass ratio. We compared our single-lined spectra with a grid of synthetic spectra and estimated the temperature of the stars. We modeled the V-band light curve with a fitting method based on the simplex algorithm, which includes an accretion disc. To constrain the main stellar parameters we fixed the mass ratio and donor temperature to the values obtained by our spectroscopic analysis. Results. We obtain a spectroscopic mass ratio q = 0.31 ± 0.03 together with donor and gainer masses M d = 2.2 ± 0.2 M , M g = 7.3 ± 0.3 M , the radii R d = 8.4 ± 0.2 R , R g = 3.6 ± 0.2 R and temperatures T d = 9400 ± 100 K, T g = 18 500 ± 500 K for the stellar components. We find that DQ Vel is a semi-detached system consisting of a B3V gainer and an A1III donor star plus an extended accretion disc around the gainer. The disc is filling 89% of the gainer Roche lobe with a temperature of 6580 ± 300 K at the outer radius. It has a concave shape that is thicker at its edge (d e = 0.6 ± 0.1 R ) than at its centre (d c = 0.3 ± 0.1 R ). We find a significant sub-orbital frequency of 0.19 d −1 in the residuals of the V-band light curve, which we interpret as a pulsation of an slowly pulsating B-type (SPB) of a gainer star. We also estimate the distance to the binary (d ∼ 3.1 kpc) using the absolute radii, apparent magnitudes, and effective temperatures of the components found in our study.

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Section: Introductionmentioning

confidence: 99%

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

Barría

Mennickent

Schmidtobreick

et al. 2013

A&A

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“…Moreover, the temperatures measured at the outer edge of the disk are far below those calculated with this assumption. Unfortunately, an evaluation of the temperature at the outer edge has only been reported in the case of AU Mon (Djurasevic et al 2010). Using their numbers the following is obtained…”

Section: Modeling the Diskmentioning

confidence: 99%

“…Disk luminosities for SW Cyg and TT Hya are taken from Albright & Richards (1996). The outer edge temperature of AU Mon is from Djurasevic et al (2010). Other characteristic disk temperatures are from Miller et al (2007) for TT Hya, from Harmanec (2002) and Ak et al (2007) for β Lyr and from Wilson & Caldwell (1978) …”

Section: Observationsmentioning

confidence: 99%

Accretion disks in Algols: Progenitors and evolution

Greve

2016

A&A

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Context. There are only a few Algols with measured accretion disk parameters. These measurements provide additional constraints for tracing the origin of individual systems, narrowing down the initial parameter space. Aims. We investigate the origin and evolution of six Algol systems with accretion disks to find the initial parameters and evolutionary constraints for them. Methods. With a modified binary evolution code, series of close binary evolution are calculated to obtain the best match for observed individual systems. Results. Initial parameters for six Algol systems with accretion disks were determined matching both the present system parameters and the observed disk characteristics. Conclusions. When Roche lobe overflow (RLOF) starts during core hydrogen burning of the donor, the disk lifetime was found to be short. The disk luminosity is comparable to the luminosity of the gainer during a large fraction of the disk lifetime.

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“…In addition, we set the gravity darkening coefficient and the albedo of the gainer and the donor to β 1,2 = 0.25 and A 1,2 = 1.0 in accordance with von Zeipel's law for radiative envelopes (Von Zeipel 1924) and complete re-radiation (Rafert & Twigg 1980). The limb-darkening for the components was calculated in the way described by Djurašević et al (2010).…”

Section: The Fitting Proceduresmentioning

confidence: 99%

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

Mennickent

Djurašević

Cabezas

et al. 2015

Monthly Notices of the Royal Astronomical Society

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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.

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Accretion disc in the eclipsing binary AU Mon★

Cited by 23 publications

References 32 publications

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

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

Accretion disks in Algols: Progenitors and evolution

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

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