Abstract
We investigate whether the Wind Compressed Disk (WCD) model can reproduce the spectral energy distribution of B[e] stars. In particular, we model the LMC B[e] star R126. Using a Monte Carlo radiative equilibrium and radiation transport code, we calculate the dust condensation radius, the 2-D temperature distribution, and the emergent flux as a function of viewing angle for a WCD model geometry. We find that the WCD model is consistent with the observational data if the dust is composed of hydrogenated amorphous carbon instead of an MRN mixture containing silicates. We also determine a criterion for dust condensation and show that the densities in the WCD outflow are large enough to form dust while spherically symmetric winds cannot form dust. This explains why B[e] stars have dust emission while normal supergiants do not.
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Bjorkman, J.E. (1998). Wind-Compressed Disks and Dust Formation in B[e] Stars. In: Hubert, A.M., Jaschek, C. (eds) B[e] Stars. Astrophysics and Space Science Library, vol 233. Springer, Dordrecht. https://doi.org/10.1007/978-94-015-9014-3_22
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DOI: https://doi.org/10.1007/978-94-015-9014-3_22
Publisher Name: Springer, Dordrecht
Print ISBN: 978-90-481-5080-9
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