Volume 551, March 2013
|Number of page(s)||11|
|Section||Interstellar and circumstellar matter|
|Published online||22 February 2013|
School of Physics & Astronomy, University of Leeds,
2 European Southern Observatory, 19001 Casilla, Santiago 19, Chile
Received: 7 August 2012
Accepted: 17 December 2012
Context. IRC +10 420 is one of the few known massive stars in rapid transition from the red supergiant phase to the Wolf-Rayet or luminous blue variable phase.
Aims. The star has an ionised wind and using the Brγ line we assess the mass-loss on spatial scales of ~1 AU.
Methods. We present new VLT Interferometer AMBER data which are combined with all other AMBER data present in the literature. The final dataset covers a position angle range of ~180° and baselines up to 110 m. The spectrally dispersed visibilities, differential phases and line flux are conjointly analysed and modelled. We also present the first AMBER/FINITO observations which cover a larger wavelength range and allow us to observe the Na i doublet at 2.2 μm. The data are complemented by X-Shooter data, which provide a higher spectral resolution view.
Results. The Brγ emission line and the Na i doublet are both spatially resolved. After correcting the AMBER data for the fact that the lines are not spectrally resolved, we find that Brγ traces a ring with a diameter of 4.18 mas, in agreement with higher spectral resolution data. We consider a geometric model in which the Brγ emission emerges from the top and bottom rings of an hour-glass shaped structure, viewed almost pole-on. It provides satisfactory fits to most visibilities and differential phases. The fact that we detect line emission from a neutral metal like Na i within the ionised region, a very unusual occurrence, suggests the presence of a dense pseudo-photosphere.
Conclusions. The ionised wind can be reproduced with a polar wind, which could well have the shape of an hour-glass. Closer in, the resolved Na i emission is found to occur on scales barely larger than the continuum. This fact and that many yellow hypergiants exhibit this comparatively rare emission hints at the presence of a “Yellow” or even “White Wall” in the Hertzsprung-Russell diagram, preventing them from visibly evolving to the blue.
Key words: stars: evolution / stars: mass-loss / supergiants / stars: individual: IRC +10 420 / circumstellar matter
Based on observations at ESO, and in particular with VLTI, proposals 079.D-0123(A), and 383.C-0166(A) and X-Shooter, proposal SV-9434.
FITS files are available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/551/A69
© ESO, 2013
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