Unified Models and Instabilities of Protoplanetary Disks

Details Unified Models and Instabilities of Protoplanetary Disks Unified Models and Instabilities of Protoplanetary Disks

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hst..prop.9514c&link_type=abstract

HST Proposal ID #9514

Physics

Hst Proposal Id #9514 Star Formation

Scientific paper

Dusty disks surrounding young stars contain the raw material from which planets form. Both terrestrial planets and giant planet cores are built of silicates and ices that begin as circumstellar dust. How much condensable material resides in these disks and how is it distributed spatially? What is the range in grain sizes? What is the dust temperature field? We propose a theoretical investigation to answer these questions using state-of-the-art radiative transfer models. Our input data includes scattered light images obtained with the Hubble Space Telescope {HST}, the thermal spectral energy distribution {SED}, and mid-infrared and millimeter-wave maps. By combining these data sets under a unified multi-wavelength analysis, we break degeneracies in fitted disk parameters that arise when using data from a single bandpass. We propose further to explain the surprisingly rippled surface geometry of the disk surrounding TW Hydra, as measured with HST by Krist et al. {2000}. Externally irradiated disks may be susceptible to the spontaneous growth of ripples in their photospheres. We ask whether ripples can amplify to the point where certain disk annuli are shadowed from central starlight, and whether they can transport angular momentum. Our investigations find direct application to the T Tauri systems TW Hya, GM Aur, HH 30, Haro 6-5b, and HK Tau/c, all of which have been extensively observed by HST.

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