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Astromineralogy of protoplanetary disks

Published online by Cambridge University Press:  01 October 2007

O. Schütz
Affiliation:
European Southern Observatory, Alonso de Cordova 3107, Santiago 19, Chile
G. Meeus
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany
M. F. Sterzik
Affiliation:
European Southern Observatory, Alonso de Cordova 3107, Santiago 19, Chile
E. Peeters
Affiliation:
The University of Western Ontario, London, ON N6A 3K7, Canada SETI Institute, 515 N. Whisman Road, Mountain View, CA 94043, USA
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Abstract

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We review mid-infrared N-band spectra (8–13 μm) for a sample of 28 targets, obtained with the TIMMI2 camera at La Silla Observatory. The sample contains 5 FU Orionis stars, 6 Herbig Ae/Be objects, 7 T Tauri stars and 10 Vega-type main sequence objects. All targets show infrared excess, but for several the proof of circumstellar matter was lacking up to our observations. We model the N-band emission features with a mixture of silicates consisting of different grain sizes and composition, and determine the status of dust processing in these disks. While for some targets the emission spectrum resembles those of known pre-main sequence stars of evolved dust, other objects show strong isolated PAH bands but no silicate emission. For the first time we find evidence of PAH processing occurring in a T Tauri star. The Vega-type object HD 113766 exhibits highly-processed secondary generation dust, likely released by the collision of planetesimal-sized bodies. The findings of our dust analysis are set in context to previous dust studies of young stellar objects.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2008

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