@inproceedings{oai:jaxa.repo.nii.ac.jp:00020690,
 author = {Lykawka, Patryk Sofia and 向井, 正 and Lykawka, Patryk Sofia and Mukai, Tadashi},
 book = {第36回月・惑星シンポジウム, Proceedings of the 36th ISAS Lunar and Planetary Symposium},
 month = {Nov},
 note = {The transneptunian belt is believed to be composed of the remnants of planetesimal accretion in the outer solar system. In the classical region (from semimajor axis a 42 AU to 48 AU), several features can be observed such as an unexpected excitation in both eccentricity e and inclination i, dynamically distinct populations and the presence of chaotic regions. The latter is usually associated with mean motion resonances with Neptune. For instance, there is evidence of a decrease of the number of objects around the 7:4 mean motion resonance (a approximately equal to 43.7 AU). In order to better understand these characteristics pointed above, numerical simulation results are presented. Test particles located initially between a = 43.0 AU and 44.4 AU with the relation of 0 less than e less than 0.30 and inclinations up to 15 deg were integrated for 2 Gy under the gravitational influence of the four giant planets. The simulated bodies seem to avoid staying locked in resonance creating a swallow gap. Inside the resonance region there is a tendency of objects with moderate to high inclinations. A chaotic diffusion experiment was also conducted to investigate the resonance dynamics. Inclination dependence and resonance dynamics in the classical region demonstrate that it is continuously evolving, causing non-negligible mixing of bodies with different inclinations., 資料番号: AA0046650041},
 pages = {161--164},
 publisher = {宇宙航空研究開発機構宇宙科学研究本部, Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA/ISAS)},
 title = {The 7:4 mean motion resonance and dynamical structures in the classical transneptunian belt},
 year = {2003}
}