Other
Scientific paper
Apr 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008acasn..49..179l&link_type=abstract
Acta Astronomica Sinica, vol. 49, no. 2, p. 179-191
Other
Methods: Numerical, Kuiper Belt, Celestial Mechanics, Solar System: Formation
Scientific paper
The Kuiper Belt is a disk of small icy objects orbiting the Sun beyond Neptune,
and the region between 40-48AU in the Kuiper Belt is supposed to consist of 'cold'
objects on low inclination orbits, which is called the classical Kuiper Belt. But recently,observations show that a `hot' population whose inclinations can be as large as 30dg reside in this classical Kuiper Belt, and the secular resonance sweeping mechanism is a probable explanation: the residual solar nebula gas dispersal can cause secular resonance sweeping (SRS), when the location of a secular resonance crosses the classical Kuiper Belt, the inclinations of the classical Kuiper Belt objects (KBOs) can be pumped up. The inclination excitation due to SRS has been investigated in detail in the compact configuration of the solar system (the orbits of four giant planets are closer to each other). It is shown that the inclination excitation depends sensitively on the angle δ between the midplane of nebula gas and the invariable plane of solar system. If the midplane of nebula gas is coplanar with the invariable plane, i.e., δ = 0, the inclination excitation is very small. But if the midplane of nebula gas is placed in the ecliptic plane, i.e., δ≈1.6°,the inclinations of the classical KBOs can attain values above 30°, as long as the residual nebula gas's density is about 1% of the minimum mass nebula model and the dissipation timescale is around 1.7-107 years (e.g. T Tauri stars).Besides, by simulating the cases of more inclined Jupiter with respect to the invariable plane, and SRS along with the migration of giant planets, we show that the effects of both cases are much less than δ for exciting the inclinations of the classical KBOs.
Li Jiying
Sun Yi-Sui
Zhou Ye-Ling
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