Earth Planets Space, Vol. 62 (No. 1), pp. 111-116, 2010
Hiroshi Kimura1, Misato Fukagawa2, Motohide Tamura3,4, Hiroshi Kobayashi1, Tetsuo Yamamoto1, Miki Ishii5, and Hiroshi Suto3
1Institute of Low Temperature Science, Hokkaido University, Kita-ku Kita-19 Nishi-8, Sapporo 060-0819, Japan
2Division of Particle and Astrophysical Sciences, Graduate School of Science, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan
3National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
4Department of Astronomical Science, The Graduate University for Advanced Studies, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
5Subaru Telescope, 650 N. A'ohoku Place, Hilo, HI 96720, USA
(Received July 30, 2008; Revised November 11, 2009; Accepted November 11, 2009; Online published February 12, 2010)
We report near-infrared imaging observations of the β Pic dust disk, from which we infer the orbital architecture of planetesimal belts that remain near mean motion resonances (MMRs) with a planet at 62 AU. Our results reveal that one of the previously identified planetesimal belts lies in the 2/3 MMR with the planet, similar to the resonant relation between Plutinos and Neptune. We suggest that all the previously reported planetesimal belts are located near the 2/3 MMRs of four planets whose spatial arrangements make a similar figure of Jupiter, Saturn, Uranus, and Neptune. This implies that the Solar System is a prototype of planetary systems around main-sequence stars in terms of planets' configuration, as expected from planet formation theories.
Key words: Stars: individual (β Pictoris), stars: planetary systems, planetary systems: formation, Kuiper Belt, meteors, meteoroids.