Spectroscopic patch model for massive stars using PHOEBE II and FASTWIND

Abdul-Masih, M.; Sana, H.; Conroy, Kyle E.; Sundqvist, J. O.; Prša, Andrej; Kochoska, A.; Puls, J.

doi:10.1051/0004-6361/201937341

Cited by 20 publications

(14 citation statements)

References 51 publications

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“…The full-width half-maximum (FWHM) and amplitude of all profiles were allowed to vary during the fitting as eclipses in the spectrum cause varying line strengths. Also the proximity of components B and C might cause the line shapes to vary at different phases of the orbit due to rotational distortions (Abdul-Masih et al 2020). The fitting was performed with the python lmfit package 4 .…”

Section: Line-profile Fitting (Stars B and C)mentioning

confidence: 99%

BAT99 126: A multiple Wolf-Rayet system in the Large Magellanic Cloud with a massive near-contact binary

Janssens

Shenar

Mahy

et al. 2021

A&A

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Context. BAT99 126 is a multiple system in the Large Magellanic Cloud containing a Wolf-Rayet (WR) star, which has a reported spectroscopic (orbital) period of 25.5 days and a photometric (orbital) period of 1.55 days, and hence is potentially one of the shortest WR binaries known to date. Such short-period binary systems that contain a WR star in low-metallicity environments are prime candidate progenitors of black-hole (BH) mergers. Aims. By thoroughly analysing the spectroscopic and photometric data, we aim to establish the true multiplicity of BAT99 126, to characterise the orbit(s) of the system, to measure the physical properties of its individual components, and to determine the overall evolutionary status of the system. Methods. Using newly acquired high resolution spectra taken with the Ultraviolet and Visual Echelle Spectrograph mounted on the Very Large Telescope, we measured radial velocities via cross-correlation and line-profile fitting and performed a spectral analysis of the individual components using model atmosphere codes. We estimated the age of the system and derived an evolutionary scenario for the 1.55-day system. Results. BAT99 126 comprises at least four components. The 1.55-day photometric signal originates in an eclipsing binary that consists of two O-type stars of spectral types O4 V and O6.5 V, which are both rapid rotators (295 km s −1 and 210 km s −1 , respectively). From the broad emission lines of the WR star, we derived a spectral type WN2.5-3. We further reject the previously reported 25.5-d period for the WR star and find that there is no detectable orbital motion within our uncertainties. The presence of additional narrow Si iii and O ii lines in the composite spectrum corresponds to a fourth component, a B1 V star. There is clear evidence that the B-type star shows a radial velocity variation; however, the data do not allow for a determination of the orbital parameters. The configurations of the B-type star, the WR star, and possible additional undetected components remain unknown. We derived masses for the O-type components of 36 ± 5M and 15 ± 2M , respectively, and estimated the age of the system to be 4.2 Myr. We find evidence of previous or ongoing mass-transfer between the two O-type components and infer initial masses of 23M for the O4 V star and 29M for the O6.5 V star. The O+O binary likely went through a phase of conservative mass transfer and is currently a near-contact system. Conclusions. We show that BAT99 126 is a multiple-quadruple or higher-order-system with a total initial mass of at least 160 M. The 1.55-day O+O binary most likely will not evolve towards a BH+BH merger, but instead will merge before the collapse of components to BHs.

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Section: Line-profile Fitting (Stars B and C)mentioning

confidence: 99%

BAT99 126: A multiple Wolf-Rayet system in the Large Magellanic Cloud with a massive near-contact binary

Janssens

Shenar

Mahy

et al. 2021

A&A

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“…In "close" binary systems effects such as reflection and tidal distortion need to be taken into account. Typically these can be treated by decomposing the stars into a patchwork layer, and then using 1D models to model each region (e.g., [111,112]). The spectra are then summed to produce a spectrum.…”

Section: Binariesmentioning

confidence: 99%

UV Spectroscopy of Massive Stars

Hillier

2020

Galaxies

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We present a review of UV observations of massive stars and their analysis. We discuss O stars, luminous blue variables, and Wolf–Rayet stars. Because of their effective temperature, the UV (912−3200 Å) provides invaluable diagnostics not available at other wavebands. Enormous progress has been made in interpreting and analysing UV data, but much work remains. To facilitate the review, we provide a brief discussion on the structure of stellar winds, and on the different techniques used to model and interpret UV spectra. We discuss several important results that have arisen from UV studies including weak-wind stars and the importance of clumping and porosity. We also discuss errors in determining wind terminal velocities and mass-loss rates.

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“…Since its discovery (Pickering & Bailey 1896), there were attempts to explain this effect without being possible to fully understand it, and with the years it became more likely the idea that there are several mechanisms producing this effect (Bagnuolo et al 1999;Linder et al 2007;Palate et al 2013). In the recent work of Abdul-Masih et al (2020), they present a model that takes into account the 3-dimensional surface geometry of a system to produce spectral profiles at given phases and orientations, and they could represent this effect in the HD 165052 system. Fig.…”

Section: Struve-sahade Effectmentioning

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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Spectroscopic patch model for massive stars using PHOEBE II and FASTWIND

Cited by 20 publications

References 51 publications

BAT99 126: A multiple Wolf-Rayet system in the Large Magellanic Cloud with a massive near-contact binary

BAT99 126: A multiple Wolf-Rayet system in the Large Magellanic Cloud with a massive near-contact binary

UV Spectroscopy of Massive Stars

Fundamental parameters of the massive eclipsing binary HM1 8

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