Signatures of Planets in Spatially Resolved Debris Disks

Computer Science

Scientific paper

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Scientific paper

The presence of debris disks around many main sequence stars indicate that plantesimal formation is a common by-product of the star formation process. In systems where massive planets are located interior to the dust-producing planetesimal region, the gravitational interaction of the dust particles with the planet can create structure in the dust disk. Because this structure is sensitive to long period planets, complementing a parameter space not covered by radial velocity and transit surveys, its study can help us learn about the diversity of planetary systems. In anticipation of future high-resolution high-sensitivity observations of spatially resolved debris disks with e.g. ALMA, LBT, SAFIR, TPF and JWST, we numerically calculate the 3-D equilibrium spatial density distributions of dust disks originated by a belt of planetesimals similar to the Kuiper Belt (KB) in the presence of interior giant planets in different planetary configurations (with planet masses ranging from 1-10 MJup in circular orbits with semimajor axis between 1-30 AU). For each of these modeled disks we use a 3-D radiative transfer code to obtain their brightness density distributions at different wavelengths that will help us to interpret future observations of these dusty ``fingerprints'' in terms of planetary architecture.

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