2008A&A...484..371O


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.28CET07:07:23

2008A&A...484..371O - Astronomy and Astrophysics, volume 484, 371-379 (2008/6-3)

Spatially resolved dusty torus toward the red supergiant WOH G64 in the Large Magellanic Cloud.

OHNAKA K., DRIEBE T., HOFMANN K.-H., WEIGELT G. and WITTKOWSKI M.

Abstract (from CDS):

We present N-band spectro-interferometric observations of the red supergiant WOH G64 in the Large Magellanic Cloud (LMC) using MIDI at the Very Large Telescope Interferometer (VLTI). While the very high luminosity (∼5x105L) previously estimated for WOH G64 suggests that it is a very massive star with an initial mass of ∼40M, its low effective temperature (∼3200K) is in serious disagreement with the current stellar evolution theory. WOH G64 was observed with VLTI/MIDI using the UT2-UT3 and UT3-UT4 baseline configurations. The dust envelope around WOH G64 has been spatially resolved with a baseline of ∼60m - the first MIDI observations to resolve an individual stellar source in an extragalactic system. The observed N-band visibilities show a slight decrease from 8 to ∼10µm and a gradual increase longward of ∼10µm, reflecting the 10µm silicate feature in self-absorption. This translates into a steep increase of the uniform-disk diameter from 8 to 10 µm (from 18 to 26mas) and a roughly constant diameter above 10µm. The visibilities measured at four position angles differing by ∼60° but at approximately the same baseline length (∼60m) do not show a noticeable difference, suggesting that the object appears nearly centrosymmetric. The observed N-band visibilities and spectral energy distribution can be reproduced by an optically and geometrically thick silicate torus model viewed close to pole-on. The luminosity of the central star is derived to be ∼2.8x105L, which is by a factor of 2 lower than the previous estimates based on spherical models. We also identify the H2O absorption features at 2.7 and 6µm in the spectra obtained with the Infrared Space Observatory and the Spitzer Space Telescope. The 2.7µm feature originates in the photosphere and/or the extended molecular layers, while the 6µm feature is likely to be of circumstellar origin. The lower luminosity newly derived from our MIDI observations and two-dimensional modeling brings the location of WOH G64 on the H-R diagram in much better agreement with theoretical evolutionary tracks for a 25M star. However, the effective temperature is still somewhat too cool for the theory. The low effective temperature of WOH G64 places it very close to or even beyond the Hayashi limit, which implies that this object may be experiencing unstable, violent mass loss.

Abstract Copyright:

Journal keyword(s): infrared: stars - techniques: interferometric - stars: supergiants - stars: late-type - stars: circumstellar matter - stars: individual: WOH G64

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9560 1
2 * alf Hor PM* 04 14 00.1144482 -42 17 39.723208 5.97 4.96 3.86 3.00 2.41 K2III 132 0
3 WOH G 64 Mi* 04 55 10.5252313969 -68 20 29.998470169     18.46 15.69 12.795 M7.5 82 0
4 * eta02 Pic PM* 05 04 58.0143319993 -49 34 40.203357685 8.35 6.47 5.01 3.81 2.90 K5III 45 0
5 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14993 1
6 * bet Lep ** 05 28 14.7231588 -20 45 33.987791 4.13 3.66 2.84 2.19 1.75 G5II-IIIa: 229 0
7 * alf Lep V* 05 32 43.8161188 -17 49 20.241380 3.02 2.77 2.57 2.35 2.14 F0Ib 271 0
8 * phi02 Ori PM* 05 36 54.3881859 +09 17 26.409553 5.70 5.04 4.09 3.33 2.78 G9.5IIIbFe-2.5 340 0
9 * gam02 Vol PM* 07 08 44.8636348625 -70 29 56.123442258   4.774 3.746     K0III 64 0
10 NML Cyg s*r 20 46 25.5382179476 +40 06 59.396202678   18.64 16.60     M7/8 484 0

    Equat.    Gal    SGal    Ecl

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2020.10.28-07:07:23

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