Dullemond, C. P. and Henning, Th. and Visser, R. and Geers, V. C. and van Dishoeck, E. F. and Pontoppidan, K. M. (2007) Dust sedimentation in protoplanetary disks with polycyclic aromatic hydrocarbons. Astronomy and Astrophysics, 473 (2). pp. 457-466. ISSN 0004-6361. doi:10.1051/0004-6361:20077581. https://resolver.caltech.edu/CaltechAUTHORS:20100205-093834042
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Abstract
Context. Dust sedimentation is known to affect the infrared spectra and images of disks. In particular the far-infrared emission may be reduced by strong sedimentation. However, dust grains of different sizes sediment to different depths in the disk. Spectral features of one species may thus be enhanced, while those of other species may be suppressed. Aims. Polycyclic aromatic hydrocarbons (PAHs) are among the smallest “dust grains”. We investigate how the presence of PAHs in protoplanetary disks affects the disk’s spectral energy distribution (SED) and feature strengths when the thermal (large) grains are allowed to sediment. Methods. We calculate the vertical distribution of dust grains for both the PAH “dust” and the thermal dust grains.We include vertical settling and vertical mixing via turbulence. The results are inserted into a Monte-Carlo radiative transfer code to compute the SEDs. Results. For high turbulence the sedimentation barely affects the spectrum. For low turbulence, however, the PAHs still stay well-mixed in the disk’s surface layer, while the 0.1 μm size grains sediment deep into the disk. This strongly enhances the PAH features relative to the continuum (by factors of 2 to 10), while the far-infrared flux is reduced. This predicts that sources with weak far-infrared flux have stronger PAH features, which is – at least among Herbig Ae stars – opposite to what is observed, suggesting that sedimentation is not the only factor responsible for the weak mid- to far-infrared excess in some disks. We speculate that coagulation might be a solution, reducing both the mid- to far-infrared flux and the PAH features.
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Additional Information: | © ESO 2007. Received 1 April 2007. Accepted 28 June 2007. We thank Carsten Dominik for useful comments. Astrochemistry in Leiden is supported by a NWO Spinoza grant and a NOVA grant, and by the European Research Training Network “The Origin of Planetary Systems” (PLANETS, contract number HPRN-CT-2002-00308). | ||||||||
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Subject Keywords: | accretion; accretion disks; circumstellar matter; stars : formation; stars : pre-main-sequence; infrared : stars | ||||||||
Issue or Number: | 2 | ||||||||
DOI: | 10.1051/0004-6361:20077581 | ||||||||
Record Number: | CaltechAUTHORS:20100205-093834042 | ||||||||
Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20100205-093834042 | ||||||||
Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||
ID Code: | 17394 | ||||||||
Collection: | CaltechAUTHORS | ||||||||
Deposited By: | Tony Diaz | ||||||||
Deposited On: | 10 Feb 2010 18:47 | ||||||||
Last Modified: | 08 Nov 2021 23:35 |
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