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Can a planet explain different cavity sizes for small & large dust grains in transition disks?

Published online by Cambridge University Press:  06 January 2014

Antonio Garufi ,
Henning Avenhaus  and
Sascha P. Quanz
Antonio Garufi
Affiliation:
Institute for Astronomy, ETH Zurich, Wolfgang-Pauli-Strasse27, Zurich, Switzerland email: antonio.garufi@phys.ethz.ch
Henning Avenhaus
Affiliation:
Institute for Astronomy, ETH Zurich, Wolfgang-Pauli-Strasse27, Zurich, Switzerland email: antonio.garufi@phys.ethz.ch
Sascha P. Quanz
Affiliation:
Institute for Astronomy, ETH Zurich, Wolfgang-Pauli-Strasse27, Zurich, Switzerland email: antonio.garufi@phys.ethz.ch
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Abstract

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Dissimilarities in the spatial distribution of small (μm–size) and large (mm–size) dust grains at the cavity edge of transition disks have been recently pointed out and are now under debate. We obtained VLT/NACO near-IR polarimetric observations of SAO 206462 (HD 135344B). The disk around the star shows very complex structures, such as dips and spirals. We also find an inner cavity much smaller than what is inferred from sub-mm images. The interaction between disk and orbiting companion(s) may explain this discrepancy.

Keywords

Stars: individual (SAO 206462, HD 135344B)Techniques: polarimetric
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S299: Exploring the Formation and Evolution of Planetary Systems , June 2013 , pp. 113 - 114
Copyright
Copyright © International Astronomical Union 2013 

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