Imaging the spinning gas and dust in the disc around the supergiant A[e] star HD 62623

Millour, F.; Meilland, A.; Chesneau, O.; Stee, Philippe; Kanaan, S.; Petrov, R.; Mourard, D.; Kraus, Stefan

doi:10.1051/0004-6361/201016193

Cited by 85 publications

(124 citation statements)

References 29 publications

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“…A convincing example of this equatorial mass-transfer was reported for the binary system HD 62623 (Plets et al 1995;Millour et al 2011), an A-type supergiant with a solar-mass companion orbiting with a period P = 137.9 d. The SED and spectra from this system exhibit a large infrared excess and strong emission lines, respectively, and HD 62623 is classified as A[e]/B[e] source. Recent AMBER observations have shown that the Brγ line originates in a dense disk of plasma larger than the orbit of the secondary (Millour et al 2011).…”

Section: Non-conservative Evolution Of the υ Sgr And β Lyr Systemsmentioning

confidence: 99%

“…Recent AMBER observations have shown that the Brγ line originates in a dense disk of plasma larger than the orbit of the secondary (Millour et al 2011). The kinematics in the Brγ line is most probably Keplerian, suggesting that most of the mass-transfer occurs in this system close to the orbital plane.…”

Section: Non-conservative Evolution Of the υ Sgr And β Lyr Systemsmentioning

confidence: 99%

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A large Hαline forming region for the massive interacting binaries β Lyrae and υ Sagitarii

Bonneau¹,

Chesneau²,

Mourard³

et al. 2011

A&A

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Aims. This study aims at constraining the properties of two interacting binary systems by measuring their continuum-forming region in the visible and the forming regions of some emission lines, in particular Hα, using optical interferometry. Methods. We have obtained visible medium (R ∼ 1000) spectral resolution interferometric observations of β Lyr and of υ Sgr using the VEGA instrument of the CHARA array. For both systems, visible continuum (520/640 nm) visibilities were estimated and differential interferometry data were obtained in the Hα emission line at several epochs of their orbital period. For β Lyr, dispersed visibilities and phases were also obtained in the Hβ and the HeI 6678 Å lines. Results. As expected, for baselines shorter than 60 m, the system of β Lyr is unresolved in the visible continuum, but the source associated with the Hα, the Hβ and the HeI 6678 Å lines appears to be well resolved at any orbital phase. The differential visibilities through these lines are lower during eclipses, indicating that significant emission originates close to the stars. The Hα line forming region appears to be made up of a compact source located near the orbital plane (possibly linked with the "hot point") and an extended source (i.e. ≥2 mas, i.e. 125 R ) out of the orbital plane (possibly associated to the "jet-like feature"). The υ Sgr continuum visibilities are at a similar level for short (20-25 m) and long (90-110 m) baselines. This is interpreted as the presence of an extended structure surrounding a compact bright source. No binary signal was detected, excluding a flux ratio between the stellar components of the system larger than 0.1 from 500 to 700 nm. The radius of the brightest star is estimated to be 0.33 ± 0.16 mas, i.e. 21 ± 10 R using the latest Hipparcos distance. By contrast, the Hα line forming region is very extended (i.e. ≥6 mas, i.e. 400 R ) and found to be off-center from the brightest star, following the orbital motion of the hidden companion. Conclusions. In both cases, the extension of the Hα line forming region is much larger than the size of the system, which is indicative of a non-conservative evolution. Although a large circumbinary disk surrounds the evolved system υ Sgr, storing a considerable part of the lost material, a substantial part of the Hα, Hβ, and the HeI 6678 Å line emission derives from regions perpendicular to the orbital plane of β Lyr.

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Section: Non-conservative Evolution Of the υ Sgr And β Lyr Systemsmentioning

confidence: 99%

Section: Non-conservative Evolution Of the υ Sgr And β Lyr Systemsmentioning

confidence: 99%

A large Hαline forming region for the massive interacting binaries β Lyrae and υ Sagitarii

Bonneau¹,

Chesneau²,

Mourard³

et al. 2011

A&A

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“…The mass loss process from L 2 has been discussed in many papers, e.g., Chesneau et al (2014) for a recent paper on V838 Mon, but in many cases for rotating disks rather than expanding ones (e.g., Millour et al 2011;Plets et al 1995). We here discuss only expanding rings/disks that escape from the binary system.…”

Section: Examining Equatorial Mass Lossmentioning

confidence: 99%

Forming equatorial rings around dying stars

Akashi

Sabach

Yogev

et al. 2015

Mon. Not. R. Astron. Soc.

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We suggest that clumpy-dense outflowing equatorial rings around evolved giant stars, such as in supernova 1987A and the Necklace planetary nebula, are formed by bipolar jets that compress gas toward the equatorial plane. The jets are launched from an accretion disk around a stellar companion. Using the FLASH hydrodynamics numerical code we perform 3D numerical simulations, and show that bipolar jets expanding into a dense spherical shell can compress gas toward the equatorial plane and lead to the formation of an expanding equatorial ring. RayleighTaylor instabilities in the interaction region break the ring to clumps. Under the assumption that the same ring-formation mechanism operates in massive stars and in planetary nebulae, we find this mechanism to be more promising for ring formation than mass loss through the second Lagrangian point. The jets account also for the presence of a bipolar nebula accompanying many of the rings.

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“…If spectrally dispersed interferograms are available, the wavelength-differential phases in spectral channels across emission lines can be used to derive phases of the Fourier transform of the object in spectral channels across emission lines (Petrov et al 2007;Schmitt et al 2009;Millour et al 2011;Ohnaka et al 2011Ohnaka et al , 2013Mourard et al 2015). This is possible if the phase of the Fourier transform of the object in the continuum is known (for example, if the continuum object is unresolvable) or can be derived from a continuum image reconstructed from continuum visibilities and continuum closure phases using a closure phase method.…”

Section: Differential-phase and Closure-phase Image Reconstruction Mementioning

confidence: 99%

VLTI-AMBER velocity-resolved aperture-synthesis imaging ofηCarinae with a spectral resolution of 12 000

Weigelt

Hofmann

Schertl

et al. 2016

A&A

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Context. The mass loss from massive stars is not understood well. η Carinae is a unique object for studying the massive stellar wind during the luminous blue variable phase. It is also an eccentric binary with a period of 5.54 yr. The nature of both stars is uncertain, although we know from X-ray studies that there is a wind-wind collision whose properties change with orbital phase. Aims. We want to investigate the structure and kinematics of η Car's primary star wind and wind-wind collision zone with a high spatial resolution of ∼6 mas (∼14 au) and high spectral resolution of R = 12 000. Methods. Observations of η Car were carried out with the ESO Very Large Telescope Interferometer (VLTI) and the AMBER instrument between approximately five and seven months before the August 2014 periastron passage. Velocity-resolved aperture-synthesis images were reconstructed from the spectrally dispersed interferograms. Interferometric studies can provide information on the binary orbit, the primary wind, and the wind collision.Results. We present velocity-resolved aperture-synthesis images reconstructed in more than 100 different spectral channels distributed across the Brγ 2.166 µm emission line. The intensity distribution of the images strongly depends on wavelength. At wavelengths corresponding to radial velocities of approximately −140 to −376 km s −1 measured relative to line center, the intensity distribution has a fan-shaped structure. At the velocity of −277 km s −1 , the position angle of the symmetry axis of the fan is ∼126 • . The fan-shaped structure extends approximately 8.0 mas (∼18.8 au) to the southeast and 5.8 mas (∼13.6 au) to the northwest, measured along the symmetry axis at the 16% intensity contour. The shape of the intensity distributions suggests that the obtained images are the first direct images of the innermost wind-wind collision zone. Therefore, the observations provide velocity-dependent image structures that can be used to test three-dimensional hydrodynamical, radiative transfer models of the massive interacting winds of η Car.

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Imaging the spinning gas and dust in the disc around the supergiant A[e] star HD 62623

Cited by 85 publications

References 29 publications

A large Hαline forming region for the massive interacting binaries β Lyrae and υ Sagitarii

A large Hαline forming region for the massive interacting binaries β Lyrae and υ Sagitarii

Forming equatorial rings around dying stars

VLTI-AMBER velocity-resolved aperture-synthesis imaging ofηCarinae with a spectral resolution of 12 000

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