A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY,<i>δ</i>ORIONIS Aa. III. ANALYSIS OF OPTICAL PHOTOMETRIC (<i>MOST</i>) AND SPECTROSCOPIC (GROUND-BASED) VARIATIONS

Pablo, H.; Richardson, Noel D.; Moffat, A. F. J.; Corcoran, M. F.; Shenar, T.; Benvenuto, O. G.; Fuller, Jim; Nazé, Yaël; Hoffman, Jennifer L.; Мирошниченко, А. С.; Apellániz, J. Maíz; Evans, Nancy Remage; Eversberg, Thomas; Gayley, K. G.; Gull, T. R.; Hamaguchi, Kenji; Hamann, Wolf-Rainer; Henrichs, H.F.; Hole, Tabetha; Ignace, Richard; Iping, R. C.; Lauer, J.; Leutenegger, Maurice A.; Lomax, Jamie R.; Nichols, Joy S.; Oskinova, L. M.; Owocki, Stan; Pollock, A. M. T.; Russell, Christopher M. P.; Waldron, W. L.; Buil, C.; Garrel, T.; Graham, Keith; Heathcote, Bernard; Lemoult, T.; Liu, Dong; Mauclaire, B.; Potter, M.; Ribeiro, José Pancrácio; Matthews, J. M.; Cameron, Chris; Guenther, D. B.; Kuschnig, R.; Rowe, Jason F.; Ruciński, S. M.; Sasselov, Dimitar; Weiß, W. W.

doi:10.1088/0004-637x/809/2/134

Cited by 20 publications

(5 citation statements)

References 57 publications

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“…Benvenuto et al (2002) used this formulation of apsidal motion to constrain the masses of the components of the non-eclipsing O3 V + O8 V binary HD 93205 by comparing the observed rate of apsidal motion against the predictions from a grid of theoretical models (see also Ferrero et al 2013;Pablo et al 2015, for other applications of this method). Whilst this method for constraining the masses is by construction highly model dependent and sensitive to the assumed age, it is interesting to apply it to HD 152218.…”

Section: Apsidal Motionmentioning

confidence: 99%

Apsidal motion in the massive binary HD 152218

Rauw

Rosu

Noels

et al. 2016

A&A

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Massive binary systems are important laboratories in which to probe the properties of massive stars and stellar physics in general. In this context, we analysed optical spectroscopy and photometry of the eccentric short-period early-type binary HD 152218 in the young open cluster NGC 6231. We reconstructed the spectra of the individual stars using a disentangling code. The individual spectra were then compared with synthetic spectra obtained with the CMFGEN model atmosphere code. We furthermore analysed the light curve of the binary and used it to constrain the orbital inclination and to derive absolute masses of (19.8 ± 1.5) and (15.0 ± 1.1) M . Combining radial velocity measurements from over 60 yr, we show that the system displays apsidal motion at a rate of (2.04−.24 )• yr −1 . Solving the Clairaut-Radau equation, we used stellar evolution models, obtained with the CLES code, to compute the internal structure constants and to evaluate the theoretically predicted rate of apsidal motion as a function of stellar age and primary mass. In this way, we determine an age of 5.8 ± 0.6 Myr for HD 152218, which is towards the higher end of, but compatible with, the range of ages of the massive star population of NGC 6231 as determined from isochrone fitting.

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Section: Apsidal Motionmentioning

confidence: 99%

Apsidal motion in the massive binary HD 152218

Rauw

Rosu

Noels

et al. 2016

A&A

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“…Less is known about hierarchical systems amongst massive stars. The well-known multiplet massive star system Mintaka (δ Ori, HD 36486) is bright, relatively close, and well-studied in many wavebands, including extensive observations at X-ray wavelengths Corcoran et al 2015;Nichols et al 2015;Pablo et al 2015;Shenar et al 2015). The center of the system is a triple, involving an O9.5 II primary and an early-type secondary in a fairly tight orbit of period ≈ 5.7 days.…”

Section: Discussionmentioning

confidence: 99%

An X-Ray Study of Two B+B Binaries: AH Cep and CW Cep

Ignace

Hole

Oskinova

et al. 2017

ApJ

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AH Cep and CW Cep are both early B-type binaries with short orbital periods of 1.8 d and 2.7 d, respectively. All four components are B0.5V types. The binaries are also double-lined spectroscopic and eclipsing. Consequently, solutions for orbital and stellar parameters make the pair of binaries ideal targets for a study of the colliding winds between two B stars. Chandra ACIS-I observations were obtained to determine X-ray luminosities. AH Cep was detected with an unabsorbed X-ray luminosity at a 90% confidence interval of (9 − 33) × 10L Bol , relative to the combined Bolometric luminosities of the two components. While formally consistent with expectations for embedded wind shocks, or binary wind collision, the near-twin system of CW Cep was a surprising non-detection. For CW Cep, an upper limit was determined with L X /L Bol < 10 −8 , again for the combined components. One difference between these two systems is that AH Cep is part of a multiple system. The X-rays from AH Cep may not arise from standard wind shocks nor wind collision, but perhaps instead from magnetism in any one of the four components of the system. The possibility could be tested by searching for cyclic X-ray variability in AH Cep on the short orbital period of the inner B stars.

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“…The frequencies were inferred to be of the SPB type. Another pulsating system observed using MOST is δ Ori A, which was found to show tidally perturbed g-mode oscillations at 12 different frequencies in the primary star (Pablo et al [96]).…”

Section: Mostmentioning

confidence: 99%

Space-Based Photometry of Binary Stars: From Voyager to TESS

Southworth

2021

Universe

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Binary stars are crucial laboratories for stellar physics, so have been photometric targets for space missions beginning with the very first orbiting telescope (OAO-2) launched in 1968. This review traces the binary stars observed and the scientific results obtained from the early days of ultraviolet missions (OAO-2, Voyager, ANS, IUE), through a period of diversification (Hipparcos, WIRE, MOST, BRITE), to the current era of large planetary transit surveys (CoRoT, Kepler, TESS). In this time observations have been obtained of detached, semi-detached and contact binaries containing dwarfs, sub-giants, giants, supergiants, white dwarfs, planets, neutron stars and accretion discs. Recent missions have found a huge variety of objects such as pulsating stars in eclipsing binaries, multi-eclipsers, heartbeat stars and binaries hosting transiting planets. Particular attention is paid to eclipsing binaries, because they are staggeringly useful, and to the NASA Transiting Exoplanet Survey Satellite (TESS) because its huge sky coverage enables a wide range of scientific investigations with unprecedented ease. These results are placed into context, future missions are discussed, and a list of important science goals is presented.

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A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY,δORIONIS Aa. III. ANALYSIS OF OPTICAL PHOTOMETRIC (MOST) AND SPECTROSCOPIC (GROUND-BASED) VARIATIONS

Cited by 20 publications

References 57 publications

Apsidal motion in the massive binary HD 152218

Apsidal motion in the massive binary HD 152218

An X-Ray Study of Two B+B Binaries: AH Cep and CW Cep

Space-Based Photometry of Binary Stars: From Voyager to TESS

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