Structure and properties of IRC+10216

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Title:		Structure and properties of IRC+10216
Authors:		Men'shchikov, Alexander B.; Balega, Yuri Yu.; Blöcker, Thomas; Osterbart, Roger; Weigelt, Gerd
Affiliation:		AA(Stockholm Observatory, SE--133 36 Saltsjöbaden, Sweden), AB(Special Astrophysical Observatory, Nizhnij Arkhyz, Karachaevo-Cherkesia, 357147, Russia), AC(Max-Planck-Insitut für Radioastronomie, Auf dem Hügel 69, D--53121 Bonn, Germany), AD(Max-Planck-Insitut für Radioastronomie, Auf dem Hügel 69, D--53121 Bonn, Germany), AE(Max-Planck-Insitut für Radioastronomie, Auf dem Hügel 69, D--53121 Bonn, Germany)
Journal:		Post-AGB Objects as a Phase of Stellar Evolution, Proceedings of the Torun Workshop held July 5-7, 2000. Edited by R. Szczerba and S. K. Górny. Astrophysics and Space Science Library Vol. 265, ISBN 07923-71453. Publisher: Kluwer Academic Publishers, Boston/Dordrecht/London, 2001.
Publication Date:		08/2001
Origin:		AUTHOR
Bibliographic Code:		2001pao..conf..343M

Abstract

We present selected results of the first detailed, two-dimensional radiative transfer modeling of the dusty envelope around the carbon star IRC+10216. The model reproduces very well the entire beam-matched spectral energy distribution of IRC+10216 from optical to centimeter wavelengths (at several phases of stellar luminosity), observed intensity profiles of the object at 1.25, 2.2, 10.5, 50, 100 microns, and 1.3 mm, a 10.5 micron lunar occultation intensity profile, our high-resolution J, H, K, and H-K bispectrum speckle-interferometry images, and visibilities in J, H, K, L, M, and N bands. We present a new, accurate identification of the carriers of the well-known 11.3 micron and 30 micron dust features in the spectrum of IRC+10216. The dust model found in this study can also be successfully applied to some other carbon stars exhibiting broad emission features in the 10.3--12.6 micron and 25--37 micron wavelength regions. A firm result of our modeling is that the brightest compact near-infrared peak observed in IRC+10216 is not the direct light from the underlying star. In contrast to previous suggestions, it is the radiation emitted and scattered in the optically thinner southern outflow cavity of a bipolar dense shell moving away from the central star.

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