TERRAPUB Earth, Planets and Space
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Earth Planets Space, Vol. 62 (No. 1), pp. 111-116, 2010
doi:10.5047/eps.2009.11.001

Planets in orbit around β Pictoris formed the orbital architecture of planetesimal belts?

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)

Abstract: 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.


Corresponding author E-mail: hiroshi@kitty.kobe-u.ac.jp


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