Neutral and ionised gas around the post-red supergiant IRC +10 420 at AU size scales

Oudmaijer, R. D.; Wit, W. J. de

doi:10.1051/0004-6361/201220185

Cited by 26 publications

(36 citation statements)

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“…The AMBER spectrum from HR 5171 A is characterized by a strong sodium line Na I 2.2 μm in emission and narrow CO bandheads that are partly filled by emission. A similar NaI 2.2 μm emission is also reported and discussed by Oudmaijer & de Wit (2013) on other YHGs, such as ρ Cas (Gorlova et al 2006) or IRC+10420 (Oudmaijer & de Wit 2013). This line betrays the presence of an extended region where the continuum forms inside the dense wind from the YHG, which veils the hydrostatic photosphere and may explain the unusual reddening and surprising decoupling between the photometric and spectroscopic data.…”

Section: Influence Of the Circumstellar Environmentsupporting

confidence: 80%

The yellow hypergiant HR 5171 A: Resolving a massive interacting binary in the common envelope phase

Chesneau

Meilland

Chapellier

et al. 2014

A&A

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Context. Only a few stars are caught in the very brief and often crucial stages when they quickly traverse the Hertzsprung-Russell diagram, and none has yet been spatially resolved in the mass transfer phase. Aims. We initiated long-term optical interferometry monitoring of the diameters of massive and unstable yellow hypergiants (YHG) with the goal of detecting both the long-term evolution of their radius and shorter term formation of a possible pseudo-photosphere related to proposed large mass-loss events. Methods. We observed HR 5171 A with AMBER/VLTI. We also examined archival photometric data in the visual and near-IR spanning more than 60 years, as well as sparse spectroscopic data. Results. HR 5171 A exhibits a complex appearance. Our AMBER data reveal a surprisingly large star for a YHG R * = 1315 ± 260 R (or ∼6.1 AU) at the distance of 3.6 ± 0.5 kpc. The source is surrounded by an extended nebulosity, and these data also show a large level of asymmetry in the brightness distribution of the system, which we attribute to a newly discovered companion star located in front of the primary star. The companion's signature is also detected in the visual photometry, which indicates an orbital period of P orb = 1304 ± 6 d. Modeling the light curve with the NIGHTFALL program provides clear evidence that the system is a contact or possibly over-contact eclipsing binary. A total current system mass of 39 +40 −22 M and a high mass ratio q ≥ 10 is inferred for the system. Conclusions. The low-mass companion of HR 5171 A is very close to the primary star that is embedded within its dense wind. Tight constraints on the inclination and v sin i of the primary are lacking, which prevents us from determining its influence precisely on the mass-loss phenomenon, but the system is probably experiencing a wind Roche-Lobe overflow. Depending on the amount of angular momentum that can be transferred to the stellar envelope, HR 5171 A may become a fast-rotating B[e]/luminous blue variable/Wolf-Rayet star. In any case, HR 5171 A highlights the possible importance of binaries for interpreting the unstable YHGs and for massive star evolution in general.

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Section: Influence Of the Circumstellar Environmentsupporting

confidence: 80%

The yellow hypergiant HR 5171 A: Resolving a massive interacting binary in the common envelope phase

Chesneau

Meilland

Chapellier

et al. 2014

A&A

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“…Comparison of the spectral line profiles in our spectra of V1302 Aql in 2001-2014 indicates the absence of a noticeable spectral variability, thus allowing to conclude that the hypergiant entered a phase of a slow down (or termination) of the T eff growth and approached the Yellow Void boundary, which is called the White Wall [10]. Earlier authors [36] suspected stabilization of the star's T eff based on a long-term photometric monitoring.…”

Section: Closest Analogs Of the Hypergiant V1302 Aqlmentioning

confidence: 49%

“…We observe steeper inner slopes instead, therefore the emission components are separated by an absorption. It is possible to have a combination of these two formation mechanisms as well as a double-ray version suggested in [10].…”

Section: Radial Velocities Of Various Features In 2001-2014mentioning

confidence: 99%

“…Highresolution spectroscopy is required to refine the structure and kinematics of its circumstellar envelope. The most adequate model to represent the observed kinematics is, in our opinion, the "rain" model proposed by Humphreys et al [17] even considering a bipolar model suggested later [10]. Observations with a moderate spectral resolving power, R ∼ 8000, were obtained by Humphreys et al [17] to test the model.…”

Section: Introductionmentioning

confidence: 98%

“…However, data obtained during the last two decades from various observations leave no doubts that V1302 Aql is an object at the yellow hypergiant stage (see review by Oudmaijer et al [6]) as well as later papers [9,10]. Moreover, V1302 Aql is now considered to be the most unambiguous massive Galactic object with a highest mass loss rate which undergoes a short-term evolutionary transition from a red supergiant to a Wolf-Rayet star [11].…”

Section: Introductionmentioning

confidence: 99%

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High-resolution optical spectroscopy of the yellow hypergiant V1302 Aql (=IRC+10420) in 2001–2014

Клочкова

Ченцов

Мирошниченко

et al. 2016

Mon. Not. R. Astron. Soc.

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We present the results of a study of spectral features and the velocity field in the atmosphere and the circumstellar envelope of the hypergiant V1302 Aql, the optical counterpart of the IR source IRC+10420, based on high-resolution spectroscopic observations obtained in 2001-2014. We measured radial velocities of the following types of lines: forbidden and permitted pure emissions, absorption and emission components of lines of ions, pure absorptions (e.g., He i, Si ii), and interstellar components of the Na i D-lines, K i, and DIBs. The heliocentric radial velocity measured for pure absorptions as well as for the forbidden and permitted pure emissions is close to the systemic radial velocity and equal to V r = 63.7±0.3, 65.2±0.3, and 62.0±0.4 km s −1 , respectively. Positions of the absorption components of the lines with inverse P Cyg profiles are stable and indicate the presence of clumps moving toward the star with a velocity of ∼20 km s −1 . The average radial velocity of the DIBs is V r (DIB) = 4.6±0.2 km s −1 . Comparison of the absorption lines observed in [2001][2002][2003][2004][2005][2006][2007][2008][2009][2010][2011][2012][2013][2014] and those in earlier data shows no noticeable variations. We conclude that the hypergiant reached a phase of slowing down (or termination) of the effective temperature growth and is currently located near the high-temperature boundary of the Yellow Void in the Hertszprung-Russell diagramme.

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Herschel/PACS observations of the 69μm band of crystalline olivine around evolved stars

Blommaert

Vries

Waters

et al. 2014

A&A

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Context. We present 48 Herschel/PACS spectra of evolved stars in the wavelength range of 67-72 µm. This wavelength range covers the 69 µm band of crystalline olivine (Mg 2−2x Fe (2x) SiO 4 ). The width and wavelength position of this band are sensitive to the temperature and composition of the crystalline olivine. Our sample covers a wide range of objects: from high mass-loss rate AGB stars (OH/IR stars, Ṁ ≥ 10 −5 M /yr), through post-AGB stars with and without circumbinary disks, to planetary nebulae and even a few massive evolved stars. Aims. The goal of this study is to exploit the spectral properties of the 69 µm band to determine the composition and temperature of the crystalline olivine. Since the objects cover a range of evolutionary phases, we study the physical and chemical properties in this range of physical environments. Methods. We fit the 69 µm band and use its width and position to probe the composition and temperature of the crystalline olivine. Results. For 27 sources in the sample, we detected the 69 µm band of crystalline olivine (Mg (2−2x) Fe (2x) SiO 4 ). The 69 µm band shows that all the sources produce pure forsterite grains containing no iron in their lattice structure. The temperature of the crystalline olivine as indicated by the 69 µm band, shows that on average the temperature of the crystalline olivine is highest in the group of OH/IR stars and the post-AGB stars with confirmed Keplerian disks. The temperature is lower for the other post-AGB stars and lowest for the planetary nebulae. A couple of the detected 69 µm bands are broader than those of pure magnesium-rich crystalline olivine, which we show can be due to a temperature gradient in the circumstellar environment of these stars. The disk sources in our sample with crystalline olivine are very diverse. They show either no 69 µm band, a moderately strong band, or a very strong band, together with a temperature for the crystalline olivine in their disk that is either very warm (∼600 K), moderately warm (∼200 K), or cold (∼120 K), respectively.

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Neutral and ionised gas around the post-red supergiant IRC +10 420 at AU size scales

Cited by 26 publications

References 39 publications

The yellow hypergiant HR 5171 A: Resolving a massive interacting binary in the common envelope phase

The yellow hypergiant HR 5171 A: Resolving a massive interacting binary in the common envelope phase

High-resolution optical spectroscopy of the yellow hypergiant V1302 Aql (=IRC+10420) in 2001–2014

Herschel/PACS observations of the 69μm band of crystalline olivine around evolved stars

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