Grain Growth and Global Structure of the Protoplanetary Disk Associated with the Mature Classical T Tauri Star, PDS 66

Details Grain Growth and Global Structure of the Protoplanetary Disk Associated with the Mature Classical T Tauri Star, PDS 66 Grain Growth and Global Structure of the Protoplanetary Disk Associated with the Mature Classical T Tauri Star, PDS 66

Jun 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...697.1305c&link_type=abstract

The Astrophysical Journal, Volume 697, Issue 2, pp. 1305-1315 (2009).

Astronomy and Astrophysics

Astronomy

8

Circumstellar Matter, Planetary Systems: Protoplanetary Disks, Stars: Pre-Main Sequence

Scientific paper

We present Australia Telescope Compact Array interferometric observations of the old (13 Myr), nearby (86 pc) classical T Tauri star (cTTS), PDS 66. Unresolved 3 and 12 mm continuum emission is detected toward PDS 66, and upper limits are derived for the 3 and 6 cm flux densities. The millimeter-wave data show a spectral slope flatter than that expected for interstellar medium-sized dust particles, which is evidence of grain growth. We also present HST/NICMOS 1.1 μm point-spread-function-subtracted coronagraphic imaging observations of the circumstellar environment of PDS 66. The Hubble Space Telescope observations reveal a bilaterally symmetric circumstellar region of dust scattering ~0.32% of the central starlight, declining in surface brightness as r -4.53. The light-scattering disk of material is inclined 32° ± 5° from a face-on viewing geometry, and extends to a radius of 170 AU. These data are combined with published optical and longer wavelength observations to make qualitative comparisons between the median Taurus and PDS 66 spectral energy distributions. By comparing the near-infrared emission to a simple model, we determine that the location of the inner disk radius is consistent with the dust sublimation radius (~1400 K at 0.1 AU). We place constraints on the total disk mass using a flat-disk model and find that it is probably too low to form gas giant planets according to current models. Despite the fact that PDS 66 is much older than a typical cTTS (<=5 Myr), its physical properties are not much different.

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