Multi-Wavelength Modeling of the Resolved Debris Disk around HD 107146

Details Multi-Wavelength Modeling of the Resolved Debris Disk around HD 107146 Multi-Wavelength Modeling of the Resolved Debris Disk around HD 107146

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007lyot.confe..33m&link_type=abstract

Proceedings of the conference In the Spirit of Bernard Lyot: The Direct Detection of Planets and Circumstellar Disks in the 21s

Physics

Scientific paper

The debris disk around HD 107146 offers an important opportunity to explore the morphology and physical properties of second-generation circumstellar dust disks because of its unique combination of near face-on viewing geometry and availability of resolved maps of the circumstellar emission over a broad range of wavelengths. The disk is resolved from the optical and the near-infrared, where it is imaged coronagraphically in scattered light, to the far-infrared, sub-millimeter, and millimeter, where it is seen in thermal emission. The coronagraphic observations, in particular, place strong constraints on the radial and azimuthal distribution of the circumstellar dust, and on its scattering properties. We present a unified description of the HD 107146 debris disk based on a radiative transfer model that incorporates the multi-wavelength resolved emission, spectral energy distribution, and 8-36 micron Spitzer/IRS spectrum of the star. Our model presents a self-consistent picture of the physical properties of the dust grains (size distribution, composition) and the overall morphology of the disk (inner and outer radii, density distribution). In particular, our constraint on the inner disk radius places a stringent upper limit on the semi-major axis of any potential giant planet that may be orbiting around HD 107146 and truncating its inner disk.

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