| Full text | |
| Author(s): |
Total Authors: 3
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| Affiliation: | [1] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508900 Sao Paulo - Brazil
[2] Univ N Carolina, Dept Phys & Astron, Greensboro, NC 27402 - USA
[3] Univ Toledo, Ritter Observ, Dept Phys & Astron, Toledo, OH 43606 - USA
Total Affiliations: 3
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| Document type: | Journal article |
| Source: | ASTROPHYSICAL JOURNAL; v. 721, n. 2, p. 1079-1089, OCT 1 2010. |
| Web of Science Citations: | 12 |
| Abstract | |
FS CMa type stars are a recently described group of objects with the B{[}e] phenomenon which exhibits 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 the circumstellar (CS) envelope is bimodal, composed of a slowly outflowing disklike 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 satisfactorily reproduce many observational properties of IRAS 00470+6429, including the Hi line profiles and the overall shape of the spectral energy distribution. Our adopted recipe for dust formation proved successful in reproducing the correct amount of dust formed in the CS envelope. Possible shortcomings of our model, as well as suggestions for future improvements, are discussed. (AU) | |