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24 April 2024 |
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Near-infrared spectro-interferometry of three OH/IR Stars with the VLTI/AMBER instrument | | A. E. Ruiz-Velasco
; M. Wittkowski
; A. Wachter
; K.-P. Schroeder
; T. Driebe
; | | Date: |
24 Oct 2011 | | Abstract: | We investigate the molecular and dusty environment of OH/IR stars in order to
characterize the mass-loss process during the tip-AGB superwind phase.
Employing the AMBER instrument at the VLT Interferometer we obtained
near-infrared H- and K-band spectro-interferometric observations of the three
OH/IR stars IRAS 13479-5436, IRAS 14086-6907 and IRAS 17020-5254 with a
spectral resolution of about 35. We use a two-component geometrical model,
consisting of a uniform disk and a Gaussian disk, to obtain characteristic
angular sizes of the central stellar sources and their dust envelopes, as well
as the flux ratios between these components. Angular uniform disk diameters of
the three central components of the objects above have values between 3.2 mas
and 5.4 mas. For their dust envelopes, we find FWHM values between 17.1 mas and
25.2 mas. According to distance estimates from the literature, the central
stellar components have radii between 900 R_sun and 1400 R_sun, while their
dust envelopes reach FWHM values between 9000 R_sun and 13000 R_sun. The
visibility functions of all three sources exhibit wavelength variations that
resemble those of earlier VLTI/AMBER observations of semi-regular and Mira
variable AGB stars. These are interpreted as characteristic of atmospheric
molecular layers lying above the photosphere. We also find that the dust
envelopes have a clearly larger optical depth than those known for Mira stars.
We interpret this as an expected result of the "superwind" phase, the final 10
000 to 30 000 years of AGB-evolution, when the mass-loss rate increases by a
factor of 10-100. By their different optical depths, the three dust shells
studied here may represent different stages of the "superwind" and different
initial masses. | | Source: | arXiv, 1110.5340 | | Services: | Forum | Review | PDF | Favorites | |
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