Disks in Transition Around Pre-Main Sequence Stars

Details Disks in Transition Around Pre-Main Sequence Stars Disks in Transition Around Pre-Main Sequence Stars

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.7602e&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #76.02; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

Circumstellar disks are essential in the evolution of stars and planets. It is believed that the formation of these disks is a natural outcome of the star formation process and that with time the disk becomes the principle supplier of the material that eventually makes up a star as well as the solids that eventually coalesce into planetary systems, much like our own solar system.
The finer details of how circumstellar disks evolve are still debated. The way in which the disk material dissipates is not well understood, specifically with regard to the physical processes which lead to the disappearance of the inner regions of a disk, a characteristic observed in transition disks. Transition disks have characteristics that fall between those objects that have clear evidence for disks and those objects with no disk material. Given that circumstellar disks are most easily detected in the infrared, the Spitzer Space Telescope has dramatically improved the ability to identify and study these objects by giving us detailed spectral energy distributions (SEDs) for pre-main sequence stars in the wavelength range 3.6-35 μm, corresponding to regions ˜0.1-5 AU from the central star. With our disk modeling codes, we can model the SEDs of these objects, providing important constraints on disk evolution and here we will present our results.

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