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Diffraction-limited 76 mas speckle-masking interferometry of the carbon star IRC+10 216 and related AGB objects with the SAO 6 m telescope

Published online by Cambridge University Press:  25 May 2016

G. Weigelt ,
T. Blöcker ,
K.-H. Hofmann ,
R. Osterbart ,
Y.Y. Balega ,
A. J. Fleischer  and
J. M. Winters
G. Weigelt
Affiliation:
Max–Planck–Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
T. Blöcker
Affiliation:
Max–Planck–Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
K.-H. Hofmann
Affiliation:
Max–Planck–Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
R. Osterbart
Affiliation:
Max–Planck–Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
Y.Y. Balega
Affiliation:
Special Astrophysical Observatory, Nizhnij Arkhyz, Karachaevo–Cherkesia, 357147, Russia
A. J. Fleischer
Affiliation:
Technische Universität Berlin, Institut für Astronomie und Astrophysik, 10623 Berlin, Germany
J. M. Winters
Affiliation:
Technische Universität Berlin, Institut für Astronomie und Astrophysik, 10623 Berlin, Germany

Abstract

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We present high-resolution J–, H–, and K–band observations of the carbon star IRC+10 216. The images were reconstructed from 6 m telescope speckle interferograms using the speckle masking bispectrum method. The H image has the unprecedented resolution of 70 mas. The H and K images consist of at least five dominant components within a 0.21 arcsec radius and a fainter asymmetric nebula. The J-, H-, and K—band images seem to have an X-shaped bipolar structure. A comparison of our images from 1995, 1996, 1997, and 1998 shows that the separation of the two brightest components A and B increased from ∼ 193 mas in 1995 to ∼ 246 mas in 1998.

The cometary shapes of component A in the H and J images and the 0.79 μm and 1.06 μm HST images suggest that the core of A is not the central star, but the southern (nearer) lobe of the bipolar structure. The position of the central star is probably at or near the position of component B, where the H—K color has its largest value of H—K = 4.2.

If the star is located at or near B, then the components A, C, and D are located close to the inner boundary of the dust shell at separations of ∼200 mas ∼30 AU (projected distance) ∼6 stellar radii for a distance of ∼ 150 pc, in agreement with our 2-dimensional radiative transfer modelling.

In addition to IRC+ 10 216 we studied the stellar disks and the dust shells of several related objects. Angular resolutions of 24 mas at 700 nm or 57 mas 1.6 μm were achieved.

Type
Part 3. Formation, Composition, and Processing of Dust
Information
Symposium - International Astronomical Union , Volume 191: Asymptotic Giant Branch Stars , 1999 , pp. 273 - 278
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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