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Evidence for a developing gap in a 10 Myr old protoplanetary disk | | Nuria Calvet
; Paola D’Alessio
; Lee Hartmann
; David Wilner
; Andrew Walsh
; Michael Sitko
; | | Date: |
25 Dec 2001 | | Subject: | astro-ph | | Affiliation: | CFA), Paola D’Alessio (IAUNAM, AMNH), Lee Hartmann (CFA), David Wilner (CFA), Andrew Walsh (Max Planck, Bonn), and Michael Sitko (Univ. of Cincinnati | | Abstract: | We have developed a self-consistent model of the disk around the nearby 10 Myr old star TW Hya which matches the observed spectral energy distribution and 7mm images of the disk. The model requires a significant dust size evolution and a partially-evacuated inner disk region, as predicted by theories of planet formation. The outer disk, which extends to at least 140 AU in radius, is very optically thick at IR wavelengths and quite massive ~0.06 Msun for the relatively advanced age of this T Tauri star. This implies long viscous and dust evolution timescales, although dust must have grown to sizes of order ~1cm to explain the sub-mm and mm spectral slopes. In contrast, the negligible near-infrared excess emission of this system requires that the disk be optically thin inside ~4 AU.This inner region cannot be completely evacuated; we need ~0.5 lunar mass of ~1 micron particles remaining to produce the observed 10 micron silicate emission. Our model requires a distinct transition in disk properties at ~4 AU, separating the inner and outer disk. The inner edge of the optically-thick outer disk must be heated almost frontally by the star to account for the excess flux at mid-IR wavelengths. We speculate that this truncation of the outer disk may be the signpost of a developing gap due to the effects of a growing protoplanet; the gap is still presumably evolving because material still resides in it, as indicated by the silicate emission, the molecular hydrogen emission, and by the continued accretion onto the central star (albeit at a much lower rate than typical of younger T Tauri stars). TW Hya thus may become the Rosetta stone for our understanding of the evolution and dissipation of protoplanetary disks. | | Source: | arXiv, astro-ph/0201425 | | Services: | Forum | Review | PDF | Favorites | |
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