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Дата индексирования: Tue Oct 2 07:08:48 2012
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Поисковые слова: galaxy cluster
Bispectrum speckle interferometry and future long-baseline interferometry of the carbon star IRC+10216

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Title:
Bispectrum speckle interferometry and future long-baseline interferometry of the carbon star IRC+10216
Authors:
Bloecker, Thomas; Balega, Yuri; Hofmann, Karl-Heinz; Men'shchikov, Alexander B.; Weigelt, Gerd; Winters, Jan-Martin
Affiliation:
AA(Max-Planck-Institut fuer Radioastronomie (Germany)), AB(Special Astrophysical Observatory (Russia)), AC(Max-Planck-Institut fuer Radioastronomie (Germany)), AD(Max-Planck-Institut fuer Radioastronomie (Germany)), AE(Max-Planck-Institut fuer Radioastronomie (Germany)), AF(Max-Planck-Institut fuer Radioastronomie (Germany))
Journal:
Interferometry for Optical Astronomy II. Edited by Wesley A. Traub . Proceedings of the SPIE, Volume 4838, pp. 1055-1060 (2003). (SPIE Homepage)
Publication Date:
02/2003
Origin:
SPIE
Abstract Copyright:
(c) 2003: SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.
Bibliographic Code:
2003SPIE.4838.1055B

Abstract

We present near-infrared (JHK) bispectrum speckle-interferometry monitoring of IRC+10216 obtained with the SAO 6m telescope. The present speckle observations covering baselines up to 6m provide important complementary informations for future long-baseline interferometry. To disentangle the apparent motions of the various IRC+10216 components and to reveal the location of the central star, future high-resolution observations are of utmost value for the interpretation of this astrophysical key object. The J-, H-, and K-band resolutions of our speckle observations are 50 mas, 56 mas, and 73 mas, resp. The K-band observations cover 8 different epochs from 1995 to 2001 and show the dynamical evolution of the dust shell which consists of several compact components within a 200 milli-arcsecond radius. Our recent two-dimensional radiative transfer modelling has shown that the central star is probably not located at the brightest dust-shell component A but at the position of the northern component B. The bright and compact component A is the southern lobe of a bipolar structure. The changes of the dust-shell structure can be related to corresponding changes of the optical depth caused, for instance, by mass-loss variations. The present observations are consistent with the predictions of hydrodynamical models that enhanced dust formation takes place on a timescale of several pulsational cycles.
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