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Issue A&A
Volume 453, Number 1, July I 2006
Page(s) 301 - 307
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20054463



A&A 453, 301-307 (2006)
DOI: 10.1051/0004-6361:20054463

Radio continuum monitoring of the extreme carbon star IRC+10216

K. M. Menten1, M. J. Reid2, E. Krügel1, M. J. Claussen3 and R. Sahai4

1  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
    e-mail: kmenten,p309ekr@mpifr-bonn.mpg.de
2  Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
    e-mail: reid@cfa.harvard.edu
3  National Radio Astronomy Obsrvatory, Array Operations Center, PO Box O, Socorro, NM 87801, USA
    e-mail: mclausse@nrao.edu
4  Jet Propulsion Laboratory, MS 183-900, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
    e-mail: raghvendra.sahai@jpl.nasa.gov

(Received 2 November 2005 / Accepted 15 March 2006 )

Abstract
We describe Very Large Array observations of the extreme carbon star IRC+10216 at 8.4, 14.9, and 22.5 GHz made over a two year period. We find possible variability correlated with the infrared phase and a cm- to sub-millimeter wavelength spectral index very close to 2. The variability, observed flux densities, and upper limit on the size are consistent with the emission arising from the stellar photosphere or a slightly larger radio photosphere.


Key words: stars: carbon -- stars: AGB and post-AGB -- radio continuum: stars -- techniques: interferometic



© ESO 2006


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