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      A giant planet imaged in the disk of the young star Beta Pictoris

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          Abstract

          Here we show that the ~10 Myr Beta Pictoris system hosts a massive giant planet, Beta Pictoris b, located 8 to 15 AU from the star. This result confirms that gas giant planets form rapidly within disks and validates the use of disk structures as fingerprints of embedded planets. Among the few planets already imaged, Beta Pictoris b is the closest to its parent star. Its short period could allow recording the full orbit within 17 years.

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          A planetary system as the origin of structure in Fomalhaut's dust belt

          James R. Graham, Mark Clampin, Paul Kalas (2005)
          The Sun and >15 percent of nearby stars are surrounded by dusty debris disks that must be collisionally replenished by asteroids and comets, as the dust would otherwise be depleted on <10 Myr timescales (ref. 1). Theoretical studies show that disk structure can be modified by the gravitational influence of planets (ref. 2-4), but the observational evidence is incomplete, at least in part because maps of the thermal infrared emission from disks have low linear resolution (35 AU in the best case; ref. 5). Optical images provide higher resolution, but the closest examples (AU Mic and Beta Pic) are edge-on (ref. 6,7), preventing the direct measurement of azimuthal and radial disk structure that is required for fitting theoretical models of planetary perturbations. Here we report the detection of optical light reflected from the dust grains orbiting Fomalhaut (HD 216956). The system is inclined 24 degrees away from edge-on, enabling the measurement of disk structure around its entire circumference, at a linear resolution of 0.5 AU. The dust is distributed in a belt 25 AU wide, with a very sharp inner edge at a radial distance of 133 AU, and we measure an offset of 15 AU between the belt's geometric centre and Fomalhaut. Taken together, the sharp inner edge and offset demonstrate the presence of planet-mass objects orbiting Fomalhaut.
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            Publication date Created: 16 June 2010
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            DOI: 10.1126/science.1187187
            ArXiV ID: 1006.3314
            SO-VID: a996df3d-b4c6-44e0-8790-b4822192cf92
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            http://arxiv.org/licenses/nonexclusive-distrib/1.0/

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            Comments 4 pages, 2 figures. Published online 10 June 2010; 10.1126/science.1187187. To appear in Science
            Categories astro-ph.EP

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