High-Resolution Imaging and Modeling of Circumstellar Debris: Architectures of Planetary Systems

Details High-Resolution Imaging and Modeling of Circumstellar Debris: Architectures of Planetary Systems High-Resolution Imaging and Modeling of Circumstellar Debris: Architectures of Planetary Systems

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20911001f&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #110.01; Bulletin of the American Astronomical Society,

Physics

Optics

Scientific paper

Circumstellar debris disks consist of dust freshly generated by the attrition and evaporation of primitive asteroids and comets. They are analogs to our Kuiper Belt and therefore inform the the architecture of trans-Neptunian space around other stars. We wish to study the diversity of these planetary systems around stars of different masses. I present high-resolution observations of debris disks, both imaging of their scattered light with adaptive optics coronagraphy, and of thermal emission in the mid-IR. AU Microscopii is a nearby M dwarf with such a disk. Coronagraphic Keck Adaptive Optics images processed with my speckle-suppression algorithm show a blue color, from optical to the near-IR, with a blue color gradient in the disk beyond 35 AU. I discuss a Monte Carlo radiative transfer code to simultaneously model the scattered light colors and SED. I compare a multi-zoned model of the grain size and space distributions to the physical model of Strubbe & Chiang (2006). In this scenario, a ring of parent bodies at 40 AU produces dust which diffuses into an outer extended disk due to stellar wind and radiation pressure. Comparison of the scattered light modeling to measurements of the disk in polarized light indicates the dust grains must be porous. I also present the first mid-IR images of warm dust grains around the Beta Pic analog HD 32297 (A0V). The structure of the thermal emission indicates an optically thin ring of grains at 65 AU. A ring of parent bodies at this location may be responsible for the production of small, warm grains. I also present high-resolution near-IR Keck imaging of the scattered light disk, which is blue in color. Like in AU Mic, the outward diffusion of these small grains from the ring may be responsible for the disk's scattered light color.

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