Abstract
The Infrared Spatial Interferometer (ISI) of the University of California at Berkeley is a two telescopes interferometer operating in the infrared (9–12 microns). Many late type stars and their circumstellar dust shell have been observed and modelled. Several results have been obtained: location of the inner radii of the dust shell, physical conditions in the dust formation zone, optical depth of the shell, diameters of some evolved stars, location of SiO masers by regard to the dust (Danchi et al. 1994a, Greenhill et al. 1995).
We detail some of the results obtained on the carbon star IRC +10216 and on the Mira type star o Ceti. This latter study combines the ISI visibility measurements and the COMEON+ adaptive optics observations in J, H and K infrared bands (1.25, 1.65 and 2.2 microns) (Cruzalèbes et al. 1996). These measurements illustrate what kind of scientific research can be engaged in this field with the VLT Interferometer.
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Lopez, B., Danchi, W.C., Cruzalèbes, P., Bester, M., Townes, C.H. (1997). Study of Late Type Stars with the Infrared Spatial Interferometer of the University of California at Berkeley. In: Paresce, F. (eds) Science with the VLT Interferometer. ESO Astrophysics Symposia. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-69398-7_25
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DOI: https://doi.org/10.1007/978-3-540-69398-7_25
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