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The circumstellar environment of the FS CMa star IRAS 00470+6429

Published online by Cambridge University Press:  12 July 2011

Alex C. Carciofi
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, Cidade Universitária, 05508-900, São Paulo, SP, BRAZIL email: carciofi@usp.br
Anatoly S. Miroshnichenko
Affiliation:
Department of Physics and Astronomy, University of North Carolina at Greensboro, Greensboro, NC 27402, USA
Jon E. Bjorkman
Affiliation:
Ritter Observatory, M.S. 113, Dept. of Physics and Astronomy, University of Toledo, Toledo, OH 43606-3390, USA
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Abstract

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FS CMa type stars are a recently described group of objects with the B[e] phenomenon that exhibit strong emission-line spectra and strong IR excesses. In this paper we report the first attempt for a detailed modeling of IRAS 00470+6429, for which we have the best set of observations. Our modeling is based on two key assumptions: the star has a main-sequence luminosity for its spectral type (B2) and that the circumstellar (CS) envelope is bimodal, composed of a slowly outflowing disk-like wind and a fast polar wind. Both outflows are assumed to be purely radial. We adopt a novel approach to describe the dust formation site in the wind that employs timescale arguments for grain condensation and a self-consistent solution for the dust destruction surface. With the above assumptions we were able to reproduce satisfactorily many observational properties of IRAS 00470+6429, including the HI line profiles and the overall shape of the spectral energy distribution.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

References

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