The 7:4 mean motion resonance and dynamical structures in the classical transneptunian belt
| Autor: | Lykawka, Patryk Sofia, Mukai, Tadashi |
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| Jazyk: | angličtina |
| Rok vydání: | 2003 |
| Předmět: | |
| Zdroj: | 第36回月・惑星シンポジウム = Proceedings of the 36th ISAS Lunar and Planetary Symposium. :161-164 |
| Popis: | 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 |
| Databáze: | OpenAIRE |
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