Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 606359.0, MPI für Astronomie / Publikationen_mpia
Warm dust resolved in the cold disk around T Chamaeleontis with VLTI/AMBER
Authors:Olofsson, J.; Benisty, M.; Augereau, J. C.; Pinte, C.; Ménard, F.; Tatulli, E.; Berger, J. P.; Malbet, F.; Merín, B.; van Dishoeck, E. F.; Lacour, S.; Pontoppidan, K. M.; Monin, J. L.; Brown, J. M.; Blake, G. A.
Date of Publication (YYYY-MM-DD):2011
Journal Abbrev.:Astronomy and Astrophysics
Volume:528
Start Page:L6
Audience:Not Specified
Abstract / Description:Context. The transition between massive Class II circumstellar disks and Class III debris disks, with dust residuals, has not yet been clearly understood. Disks are expected to dissipate with time, and dust clearing in the inner regions can be the consequence of several mechanisms. Planetary formation is one of them that will possibly open a gap inside the disk. <BR /> Aims: According to recent models based on photometric observations, T Cha is expected to present a large gap within its disk, meaning that an inner dusty disk is supposed to have survived close to the star. We investigate this scenario with new near-infrared interferometric observations. <BR /> Methods: We observed T Cha in the H and K bands using the AMBER instrument at VLTI and used the MCFOST radiative transfer code to model the SED of T Cha and the interferometric observations simultaneously and to test the scenario of an inner dusty structure. We also used a toy model of a binary to check that a companion close to the star can reproduce our observations. <BR /> Results: The scenario of a close (few mas) companion cannot satisfactorily reproduce the visibilities and SED, while a disk model with a large gap and an inner ring producing the bulk of the emission (in H and K-bands) close to 0.1 AU is able to account for all the observations. <BR /> Conclusions: With this study, the presence of an optically thick inner dusty disk close to the star and dominating the H and K-bands emission is confirmed. According to our model, the large gap extends up to ~7.5 AU. This points toward a companion (located at several AU) gap-opening scenario to explain the morphology of T Cha. Based on AMBER observations collected at the VLTI (European Southern Observatory, Paranal, Chile) with open time programs 083.C-0295(A,B).
Free Keywords:stars: pre-main sequence; stars: evolution; protoplanetary disks; circumstellar matter; infrared: stars; techniques: interferometric
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://cdsads.u-strasbg.fr/abs/2011A%26A...528L......
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.