Coronagraphic Polarimetry of HST-Resolved Circumstellar T Tauri and Debris Disks.

Details Coronagraphic Polarimetry of HST-Resolved Circumstellar T Tauri and Debris Disks. Coronagraphic Polarimetry of HST-Resolved Circumstellar T Tauri and Debris Disks.

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.5016s&link_type=abstract

American Astronomical Society, AAS Meeting #211, #50.16; Bulletin of the American Astronomical Society, Vol. 39, p.814

Astronomy and Astrophysics

Astronomy

Scientific paper

The formation of planetary systems is intimately linked to the dust population in circumstellar disks, thus understanding dust grain evolution is essential to advancing our understanding of how planets form. While it is well established that stars form in ISM-like protostellar environments, the connection to now observable light-scattering circumstellar disks and the processes of planet formation is still very uncertain. Mid-IR spectral studies suggest that disk grains are growing in the environments of young stellar objects during the putative planet-formation epoch. Structures revealed in well resolved images of older circumstellar debris disks suggest gravitational influences on the disks from putative co-orbital bodies of planetary mass. To further elucidate the dust and systemic properties in potentially planet-forming systems, we have undertaken two symbiotic HST imaging programs that exploit the recently commission capabilities of coronagraphic polarimetry with the Near Infrared Camera and Multi-Object Spectrometer, probing dust structures in T Tauri circumstellar disks during the early epochs of planet formation, and debris disks around older stars. We present the first observational results from these two programs in light of earlier commission observations of TW Hya, focusing on the scattered light disks around the T Tauri star GM Aur and the debris disk associated with HR 32297, along with optical (ACS) coronagraphic polarimetry of the unusual dust structure around HD 61005.
Support for this work was provided by NASA through grant numbers GO-9768. 10847 and 10852 from the Space Telescope Science Institute, which is operated by Association of Universities for Research in Astronomy Incorporated, under NASA contract NAS5-26555.

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