TOWARD UNDERSTANDING THE B[e] PHENOMENON. IV. MODELING OF IRAS 00470+6429
- Instituto de Astronomia, Geofisica e Ciencias Atmosfericas, Universidade de Sao Paulo, Rua do Matao 1226, Cidade Universitaria, 05508-900 Sao Paulo (Brazil)
- Department of Physics and Astronomy, University of North Carolina at Greensboro, Greensboro, NC 27402 (United States)
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 H I 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.
- OSTI ID:
- 21464796
- Journal Information:
- Astrophysical Journal, Vol. 721, Issue 2; Other Information: DOI: 10.1088/0004-637X/721/2/1079; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
Similar Records
ALMA observations of the water fountain pre-planetary nebula IRAS 16342-3814: high-velocity bipolar jets and an expanding torus
THE SPATIOKINEMATICAL STRUCTURE OF H{sub 2}O AND OH MASERS IN THE ''WATER FOUNTAIN'' SOURCE IRAS 18460-0151