A new spectroscopic analysis of the massive O + O type binary HD 54662 AB

Barbá, R. H.; Sabín-Sanjulián, C.; Arias, J. I.; Gamen, R.; Morrell, N.; Ferrero, G.; Apellániz, J. Maíz; Putkuri, C.; Diaz, Sébastien; Boyajian, Tabetha S.; Fullerton, A. W.; McSwain, M. Virginia

doi:10.1093/mnras/staa927

Cited by 7 publications

(2 citation statements)

References 48 publications

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“…The RV measurements above described provide a starting point to apply a spectral disentangling method in order to obtain the individual spectra of each system's component. In this case, we implemented the method developed by González & Levato (2006), following the procedure applied by Barbá et al (2020) in the analysis of the O+O system HD 54662 AB. Compared to HD 54662 AB, HM1 8 has the advantage of presenting orbital phases for which the spectral lines of the components are clearly separated, and the profiles are not blended at all (e.g.…”

Section: Spectral Disentanglingmentioning

confidence: 99%

Fundamental parameters of the massive eclipsing binary HM1 8

Rodríguez,

Ferrero,

Benvenuto

et al. 2021

Preprint

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We present a comprehensive study of the massive binary system HM1 8, based on multi-epoch high resolution spectroscopy, 𝑉-band photometry and archival X-ray data. Spectra from the OWN Survey, a high resolution optical monitoring of Southern O and WN stars, are used to analyse the spectral morphology and perform quantitative spectroscopic analysis of both stellar components. The primary and secondary components are classified as O4.5 IV(f) and O9.7 V, respectively. From a radial-velocity (RV) study we derived a set of orbital parameters for the system. We found an eccentric orbit (𝑒 = 0.14 ± 0.01) with a period of 𝑃 = 5.87820 ± 0.00008 days. Through the simultaneous analysis of the RVs and the 𝑉-band light curve we derived an orbital inclination of 70.0 • ± 2.0 and stellar masses of 𝑀 𝑎 = 33.6 +1.4 −1.2 M for the primary, and 𝑀 𝑏 = 17.7 +0.5 −0.7 M for the secondary. The components show projected rotational velocities 𝑣 1 sin 𝑖 = 105 ± 14 km s −1 and 𝑣 2 sin 𝑖 = 82 ± 15 km s −1 , respectively. A tidal evolution analysis is also performed and found to be in agreement with the orbital characteristics. Finally, the available X-ray observations show no evidence of a colliding winds region, therefore the X-ray emission is attributed to stellar winds.

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Section: Spectral Disentanglingmentioning

confidence: 99%

Fundamental parameters of the massive eclipsing binary HM1 8

Rodríguez,

Ferrero,

Benvenuto

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…We calculated a new spectroscopic orbit using the RVs from Tramper et al (2016), along with ten new RV measurements. The reader is referred to Barbá et al (2020) for details about the reduction process. The RVs were derived through a double Gaussian fit of the He 𝜆5412 absorption line, which is clearly double in most of the spectra.…”

Section: Spectroscopic Data and Orbital Solutionmentioning

confidence: 99%

The winking eye of a hefty star. WR 21a revealed as a very massive eclipsing binary by TESS

Barbá¹,

Gamen²,

Martín-Ravelo³

et al. 2021

Preprint

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WR 21a was known as a massive spectroscopic binary composed of an O2.5 If*/WN6ha primary and an O3 V((f*))z secondary. Although a minimum value, the mass estimated for the primary placed it as one of the most massive stars found in our Galaxy. We report the discovery of photometric variations in the time series observations carried out by the Transiting Exoplanet Survey Satellite (TESS). These light variations are interpreted as formed by two main components: a sharp partial eclipse of the O3 by the O2.5/WN6 star, and tidally excited oscillations. Based on the light minima a new ephemeris for the system is calculated. The system configuration is detached and the observed eclipse corresponds to the periastron passage. During the eclipse, the light curve shape suggests the presence of the heartbeat effect. The frequencies derived for the tidally excited oscillations are harmonics of the orbital period. Combining new and previously published radial velocity measurements, a new spectroscopic orbital solution is also obtained. Using the code we model the TESS light curve and determine stellar radii of 𝑅 O2.5/WN6 = 23.3 R and 𝑅 O3 = 14.8 R and an orbital inclination 𝑖 = 61 • .8 ± 1 • .5. The latter combined with the spectroscopic minimum masses lead to absolute masses of 𝑀 O2.5/WN6 = 94.4 M and 𝑀 O3 = 53.6 M , which establishes WR 21a as belonging to the rare group of the very massive stars.

show abstract

Fundamental parameters of the massive eclipsing binary HM1 8

Rodríguez

Ferrero

Benvenuto

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present a comprehensive study of the massive binary system HM1 8, based on multi-epoch high resolution spectroscopy, V-band photometry and archival X-ray data. Spectra from the OWN Survey, a high resolution optical monitoring of Southern O and WN stars, are used to analyse the spectral morphology and perform quantitative spectroscopic analysis of both stellar components. The primary and secondary components are classified as O4.5 IV(f) and O9.7 V, respectively. From a radial-velocity (RV) study we derived a set of orbital parameters for the system. We found an eccentric orbit (e = 0.14 ± 0.01) with a period of P = 5.87820 ± 0.00008 days. Through the simultaneous analysis of the RVs and the V-band light curve we derived an orbital inclination of 70.0○ ± 2.0 and stellar masses of $M_a=33.6^{+1.4}_{-1.2}~\text{M}_{\odot }$ for the primary, and $M_b=17.7^{+0.5}_{-0.7}~\text{M}_{\odot }$ for the secondary. The components show projected rotational velocities v1sin i = 105 ± 14 km s−1 and v2sin i = 82 ± 15 km s−1, respectively. A tidal evolution analysis is also performed and found to be in agreement with the orbital characteristics. Finally, the available X-ray observations show no evidence of a colliding winds region, therefore the X-ray emission is attributed to stellar winds.

show abstract

A new spectroscopic analysis of the massive O + O type binary HD 54662 AB

Cited by 7 publications

References 48 publications

Fundamental parameters of the massive eclipsing binary HM1 8

Fundamental parameters of the massive eclipsing binary HM1 8

The winking eye of a hefty star. WR 21a revealed as a very massive eclipsing binary by TESS

Fundamental parameters of the massive eclipsing binary HM1 8

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