Properties of six short-period massive binaries: A study of the effects of binarity on surface chemical abundances

Martins, F.; Mahy, L.; Hervé, Anthony

doi:10.1051/0004-6361/201731593

Cited by 29 publications

(30 citation statements)

References 58 publications

(89 reference statements)

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“…This result confirms that the use of single-star evolutionary tracks to explain the product of binary interactions do not match. This trend was also observed by Martins et al (2017) for massive binary systems located in our Galaxy.…”

Section: Mass Discrepancysupporting

confidence: 85%

“…We can use it as a Rosetta Stone to tackle the mass-discrepancy problem. Martins et al (2017) pointed out that the evolutionary masses in their sample of six binary systems were also systematically higher by about 15-20% than the spectroscopic and dynamical masses. In Table 1, we give the dynamical, spectroscopic, and evolutionary masses for each component of the 13 systems with light curves studied in the present paper.…”

Section: Mass Discrepancymentioning

confidence: 96%

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The Tarantula Massive Binary Monitoring

Mahy

Almeida

Sana

et al. 2020

A&A

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Context. A high fraction of massive stars are found to be binaries but only a few of them are reported as photometrically variable. By studying the populations of double-lined spectroscopic binaries in the 30 Doradus region, we found a subset of them that have photometry from the OGLE project and that display variations in their light curves related to orbital motions. Aims. The goal of this study is to determine the dynamical masses and radii of the 26 binary components in order to investigate the mass-discrepancy problem and to provide an empirical mass-luminosity relation for the Large Magellanic Cloud (LMC). Methods. We use the PHOEBE programme to perform a systematic analysis of the OGLE V and I light curves obtained for 13 binary systems in the 30 Doradus region. We adopt the effective temperatures, and orbital parameters derived previously to obtain the inclinations of the systems and the parameters of the individual components. Results. Three systems display eclipses in their light curves, while the others only display ellipsoidal variations. We classify two systems as over-contact, five as semi-detached, and four as detached. The two remaining systems have uncertain configurations due to large uncertainties on their inclinations. The fact that systems display ellipsoidal variations has a significant impact on the inclination errors. From the dynamical masses, luminosities, and radii, we provide LMC-based empirical mass-luminosity and mass-radius relations, and we compare them to other relations given for the Galaxy, the LMC, and the Small Magellanic Cloud. These relations differ for different mass ranges, but do not seem to depend on the metallicity regimes. We also compare the dynamical, spectroscopic, and evolutionary masses of the stars in our sample. While the dynamical and spectroscopic masses agree with each other, the evolutionary masses are systematically higher, at least for stars in semi-detached systems. This suggests that the mass discrepancy can be partly explained by past or ongoing interactions between the stars.

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Section: Mass Discrepancysupporting

confidence: 85%

Section: Mass Discrepancymentioning

confidence: 96%

The Tarantula Massive Binary Monitoring

Mahy

Almeida

Sana

et al. 2020

A&A

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“…Mahy et al (2011) find that the Roche lobe filling component of the semidetached system LZ Cep shows a strong helium and nitrogen mass fraction enhancement. HD 149404 (Raucq et al 2016) and XZ Cep (Martins et al 2017) contain Roche lobe filling stars with surface abundances close to CNO equilibrium.…”

Section: Surface Abundancesmentioning

confidence: 99%

“…Modern observations of massive star binaries allow to determine the binary and stellar properties of individual systems in great detail (Hilditch et al 2005;Torres et al 2010;Martins et al 2017;Pavlovski et al 2018;Johnston et al 2019;Mahy et al 2020a,b). This provides ideal conditions to constrain the uncertain physics assumptions in binary evolution models (Ritchie et al 2010;Clark et al 2014;Abdul-Masih et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Detailed models of interacting short-period massive binary stars

Sen,

Langer,

Marchant

et al. 2021

Preprint

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Context. The majority of massive stars are part of binary systems. In about a quarter of these, the companions are so close that mass transfer occurs while they undergo core hydrogen burning, first on the thermal and then on the nuclear timescale. The nuclear timescale mass transfer leads to observational counterparts: the semi-detached so-called massive Algol binaries. These systems may provide urgently needed tests of the physics of mass transfer. However, comprehensive model predictions for these systems are sparse. Aims. We use a large grid of detailed evolutionary models of short-period massive binaries, and follow-up population synthesis calculations, to derive probability distributions of the observable properties of massive Algols and their descendants. Methods. Our results are based on ∼10,000 binary model sequences calculated with the stellar evolution code MESA, using a metallicity suitable for the Large Magellanic Cloud (LMC), covering initial donor masses between 10 M and 40 M and initial orbital periods above 1.4 d. These models include internal differential rotation and magnetic angular momentum transport, non-conservative mass and angular momentum transfer between the binary components, and time-dependent tidal coupling. Results. Our models imply ∼30, or ∼3% of the ∼1,000 core hydrogen burning O-star binaries in the LMC to be currently in the semidetached phase. Our donor models are up to 25-times more luminous than single stars of identical mass and effective temperature, which agrees with the observed Algols. A comparison of our models with the observed orbital periods and mass ratios implies rather conservative mass transfer in some systems, while very inefficient one in others. This is generally well reproduced by our spindependent mass transfer algorithm, except for the lowest considered masses. The observations reflect the slow increase of the surface nitrogen enrichment of the donors during the semi-detached phase all the way to CNO-equilibrium. We also investigate the properties of our models after core hydrogen depletion of the donor star, when these models correspond to Wolf-Rayet/helium+OB star binaries. Conclusions. A dedicated spectroscopic survey of massive Algol systems may allow to derive the dependence of the efficiency of thermal timescale mass transfer on the binary parameters, as well as the efficiency of semiconvective mixing in the stellar interior. This would be a crucial step towards reliable binary models up to the formation of supernovae and compact objects.

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“…The parameters γ, K, a sin i, and M sin 3 i denote the apparent systemic velocity, the semi-amplitude of the radial velocity curve, the projected distance from the center of the star to the center of mass of the binary system, and the minimum masses of the binary components, respectively. References: (1) Lindegren et al ( 2018), (2) Martins et al (2017) 2 Observations and data reduction…”

Section: Introductionmentioning

confidence: 99%

Polarization study of massive binaries with the ARIES-1.04 m telescope

Arora¹,

Pandey²,

Joshi³

et al. 2019

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We present preliminary results obtained from optical (B, V, R, and I) linear polarimetric observations of the O+O massive binary DH Cep. The observations were made on six nights in 2017 with the Aries IMaging POLarimeter (AIMPOL) mounted at the back of the 1.04-m Sampurnanand Telescope of ARIES. The average intrinsic linear polarization in each of the B, V, R, and I photometric bands is found to be less than 1%. The degree of polarization as well as the polarization angle appear to be orbital phase dependent. The significant polarization variability noticed towards shorter wavelengths (i.e. B and V bands) is indicative of the asymmetric circumstellar envelope.

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Properties of six short-period massive binaries: A study of the effects of binarity on surface chemical abundances

Cited by 29 publications

References 58 publications

The Tarantula Massive Binary Monitoring

The Tarantula Massive Binary Monitoring

Detailed models of interacting short-period massive binary stars

Polarization study of massive binaries with the ARIES-1.04 m telescope

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