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26 April 2024 |
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The dynamical evolution of the fragmented, bipolar dust shell around the carbon star IRC +10216: Rapid changes of a PPN-like structure? | | R. Osterbart
; Y. Balega
; T. Bloecker
; A. Men’shchikov
; G. Weigelt
; | | Date: |
22 Mar 2000 | | Subject: | astro-ph | | Affiliation: | Max-Planck-Institut fuer Radioastronomie, Bonn, Germany - Special Astrophysical Observatory, Nizhnij Arkhyz, Russia - Stockholm Observatory, Saltsjobaden, Sweden | | Abstract: | We present high-resolution J-, H-, and K-band observations and the first H-K color image of the carbon star IRC +10216. The images were reconstructed from 6m telescope speckle interferograms using the bispectrum speckle interferometry method. The H and K images with resolutions between 70mas and 92mas consist of several compact components within a 0.2" radius and a fainter asymmetric nebula. The brightest four components are denoted with A to D in the order of decreasing brightness in the 1996 image. A comparison of our images from 1995, 1996, 1997, and 1998 gives - almost like a movie of five frames - insight into the dynamical evolution of the inner nebula. For instance, the separation of the two brightest components A and B increased from 191 mas in 1995 to 265 mas in 1998. At the same time, component B is fading and the components C and D become brighter. The X-shaped bipolar structure of the nebula, most prominently present in the J-band image, implies an asymmetric mass loss. Such asymmetries are often present in protoplanetary nebulae but are unexpected for AGB stars. IRC +10216 is thus likely to be very advanced in its AGB evolution, shortly before turning into a protoplanetary nebula. The cometary shapes of A in the H and J images and in the 0.79 micron and 1.06 micron HST images suggest that the core of A is not the central star, but the southern lobe of a bipolar structure. The position of the central star is probably at or near the position of component B, where the H-K color has a value of 4.2. If the star is at or near B, then the components A, C, and D are likely to be located at the inner boundary of the dust shell. | | Source: | arXiv, astro-ph/0003328 | | Services: | Forum | Review | PDF | Favorites | |
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