Spectral and spatial imaging of the Be+sdO binary<i>ϕ</i>Persei

Mourard, D.; Monnier, John D.; Meilland, A.; Gies, Douglas R.; Millour, F.; Benisty, M.; Chen, Xiao; Grundstrom, E. D.; Ligi, R.; Schaefer, Gail H.; Baron, Fabien; Kraus, Stefan; Zhao, M.; Pedretti, E.; Bério, Philippe; Clausse, J. M.; Nardetto, N.; Perraut, K.; Spang, A.; Stee, Philippe; Tallon–Bosc, I.; McAlister, Harold A.; Brummelaar, T. ten; Ridgway, S. T.; Sturmann, J.; Sturmann, L.; Turner, N.; Farrington, C.

doi:10.1051/0004-6361/201425141

Cited by 76 publications

(86 citation statements)

References 69 publications

(139 reference statements)

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“…Evidence is also provided by the properties of the companion, which is a hot subdwarf O star of 1.2±0.2M (Mourard et al 2015). Its properties and current orbital period of 126 days match the theoretical expectations for a typical post-mass-transfer system.…”

Section: Direct Progenitors and Descendants Of Late Ccsnementioning

confidence: 53%

Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction

Zapartas

Mink

Izzard

et al. 2017

A&A

159

152

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Most massive stars, the progenitors of core-collapse supernovae, are in close binary systems and may interact with their companion through mass transfer or merging. We undertake a population synthesis study to compute the delay-time distribution of core-collapse supernovae, that is, the supernova rate versus time following a starburst, taking into account binary interactions. We test the systematic robustness of our results by running various simulations to account for the uncertainties in our standard assumptions. We find that a significant fraction, 15 +9 −8 %, of core-collapse supernovae are 'late', that is, they occur 50-200 Myrs after birth, when all massive single stars have already exploded. These late events originate predominantly from binary systems with at least one, or, in most cases, with both stars initially being of intermediate mass (4 − 8M ). The main evolutionary channels that contribute often involve either the merging of the initially more massive primary star with its companion or the engulfment of the remaining core of the primary by the expanding secondary that has accreted mass at an earlier evolutionary stage. Also, the total number of core-collapse supernovae increases by 14 +15 −14 % because of binarity for the same initial stellar mass. The high rate implies that we should have already observed such late core-collapse supernovae, but have not recognized them as such. We argue that φ Persei is a likely progenitor and that eccentric neutron star -white dwarf systems are likely descendants. Late events can help explain the discrepancy in the delay-time distributions derived from supernova remnants in the Magellanic Clouds and extragalactic type Ia events, lowering the contribution of prompt Ia events. We discuss ways to test these predictions and speculate on the implications for supernova feedback in simulations of galaxy evolution.

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Section: Direct Progenitors and Descendants Of Late Ccsnementioning

confidence: 53%

Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction

Zapartas

Mink

Izzard

et al. 2017

A&A

159

152

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“…Vanbeveren et al (1998) describe a probable evolutionary channel for the early Be star φ Per, which was discovered to have a hot subdwarf companion by Gies et al (1998) using ultraviolet spectroscopy. Recently, the companion has also been detected directly through interferometry (Mourard et al 2015). In the case of φ Per, Vanbeveren et al (1998) describe how a system that began its life as a 6 + 5M ⊙ with an orbital period of 13.5 d undergoes conservative Roche lobe overflow.…”

Section: Discussionmentioning

confidence: 99%

A Spectroscopic Orbit for the Late-type Be Star β CMi

Richardson

Gerhartz

Bjorkman

et al. 2017

ApJ

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The late-type Be star β CMi is remarkably stable compared to other Be stars that have been studied. This has led to a realistic model of the outflowing Be disk by Klement et al. These results showed that the disk is likely truncated at a finite radius from the star, which Klement et al. suggest is evidence for an unseen binary companion in orbit. Here we report on an analysis of the Ritter Observatory spectroscopic archive of β CMi to search for evidence of the elusive companion. We detect periodic Doppler shifts in the wings of the Hα line with a period of 170 d and an amplitude of 2.25 km s −1 , consistent with a low-mass binary companion (M ≈ 0.42M ⊙ ). We then compared the small changes in the violet-to-red peak height changes (V /R) with the orbital motion. We find weak evidence that it does follow the orbital motion, as suggested by recent Be binary models by Panoglou et al. Our results, which are similar to those for several other Be stars, suggest that β CMi may be a product of binary evolution where Roche lobe overflow has spun up the current Be star, likely leaving a hot subdwarf or white dwarf in orbit around the star. Unfortunately, no direct sign of this companion star is found in the very limited archive of International Ultraviolet Explorer spectra.

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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

Self Cite

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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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Spectral and spatial imaging of the Be+sdO binaryϕPersei

Cited by 76 publications

References 69 publications

Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction

Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction

A Spectroscopic Orbit for the Late-type Be Star β CMi

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

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