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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 710122.0, MPI für Astronomie / Publikationen_mpia
On the structure of the transition disk around TW Hydrae
Authors:Menu, J.; van Boekel, R.; Henning, T.; Chandler, C. J.; Linz, H.; Benisty, M.; Lacour, S.; Min, M.; Waelkens, C.; Andrews, S. M.; Calvet, N.; Carpenter, J. M.; Corder, S. A.; Deller, A. T.; Greaves, J. S.; Harris, R. J.; Isella, A.; Kwon, W.; Lazio, J.; Le Bouquin, J. -. B.; Ménard, F.; Mundy, L. G.; Pérez, L. M.; Ricci, L.; Sargent, A. I.; Storm, S.; Testi, L.; Wilner, D. J.
Date of Publication (YYYY-MM-DD):2014
Title of Journal:Astronomy and Astrophysics
Volume:564
Start Page:id. A93 (22 pp)
Audience:Not Specified
Abstract / Description:Context. For over a decade, the structure of the inner cavity in the transition disk of TW Hydrae has been a subject of debate. Modeling the disk with data obtained at different wavelengths has led to a variety of proposed disk structures. Rather than being inconsistent, the individual models might point to the different faces of physical processes going on in disks, such as dust growth and planet formation. <BR /> Aims: Our aim is to investigate the structure of the transition disk again and to find to what extent we can reconcile apparent model differences. <BR /> Methods: A large set of high-angular-resolution data was collected from near-infrared to centimeter wavelengths. We investigated the existing disk models and established a new self-consistent radiative-transfer model. A genetic fitting algorithm was used to automatize the parameter fitting, and uncertainties were investigated in a Bayesian framework. <BR /> Results: Simple disk models with a vertical inner rim and a radially homogeneous dust composition from small to large grains cannot reproduce the combined data set. Two modifications are applied to this simple disk model: (1) the inner rim is smoothed by exponentially decreasing the surface density in the inner ~3 AU, and (2) the largest grains (>100 mum) are concentrated towards the inner disk region. Both properties can be linked to fundamental processes that determine the evolution of protoplanetary disks: the shaping by a possible companion and the different regimes of dust-grain growth, respectively. <BR /> Conclusions: The full interferometric data set from near-infrared to centimeter wavelengths requires a revision of existing models for the
Free Keywords:protoplanetary disks; techniques: interferometric; stars: individual: TW Hya
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-6361 %R 10.1051/0004-6361/201322961
URL:http://cdsads.u-strasbg.fr/abs/2014A%26A...564A..9...
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