M. Honda, Koen Maaskant, Y. K. Okamoto, H. Kataza, M. Fukagawa, L. B. F. M. Waters, C. Dominik, A. G. G. M. Tielens, G. D. Mulders, M. Min, T. Yamashita, T. Fujiyoshi, T. Miyata, S. Sako, I. Sakon, H. Fujiwara, T. Onaka
The disk around the Herbig Ae star HD\,169142 was imaged and resolved at 18.8 and 24.5\,$\mu$m using Subaru/COMICS. We interpret the observations using a 2D radiative transfer model and find evidence for the presence of a large gap. The MIR images trace dust that emits at the onset of the strong rise in the spectral energy distribution (SED) at 20\,$\mu$m, therefore are very sensitive to the location and characteristics of the inner wall of the outer disk and its dust. We determine the location of the wall to be 23$^{+3}_{-5}$\,AU from the star. An extra component of hot dust must exist close to the star. We find that a hydrostatic optically thick inner disk does not produce enough flux in the NIR and an optically thin geometrically thick component is our solution to fit the SED. Considering the recent findings of gaps and holes in a number of Herbig Ae/Be group I disks, we suggest that such disk structures may be common in group I sources. Classification as group I should be considered a support for classification as a transitional disk, though improved imaging surveys are needed to support this speculation.
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http://arxiv.org/abs/1204.5364
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