Imaging the gap in the disk around CS Cha

Details Imaging the gap in the disk around CS Cha Imaging the gap in the disk around CS Cha

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008atnf.prop.1302l&link_type=abstract

ATNF proposal C1798, Semester: April, 2008

Physics

Stellar, Galactic, Atca

Scientific paper

The time scales over which disks around young stars dissipate, and the processes that cause the dissipation of the disks, are not very well known, and seem to differ from disk to disk. However, after 10 Myr, the vast majority of stars appear to have lost their disks. Analysis of SEDs suggests that at least two ways lead from the classical T Tauri stage with disks containing unprocessed dust to pre-main sequence stars with debris disks. From models of young stellar objects to explain the observed SEDs, it is inferred that about 10% of the disks are found in a transitional phase in which a large inner gap of several tens of AU exists. However, the infrared deficits in SEDs of accreting disks around low-mass, pre-main sequence stars can also be explained by a combination of opacity and geometry effects in the unresolved systems. We here propose to image the disk around the T Tauri star CS Cha to resolve this degeneracy. By resolving the system at two different wavelengths, we furthermore study the evolution of grain growth as a function of position in the disk, to start to differentiate between the different gap opening mechanisms.

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