Abstract
We review theoretical and numerical results obtained for secular resonant motion in the asteroidal belt. William's theory (1969) yields the locations of the principal secular resonances ν5, ν6, and ν16 in the asteroidal belt. Theories by Nakai and Kinoshita (1985) and by Yoshikawa (1987) allow us to model the basic features of orbital evolution at the secular resonances ν16 and ν6, respectively. No theory is available for the secular resonance v5. Numerical experiments by Froeschle and Scholl yield quantitative and new qualitative results for orbital evolutions at the three principal secular resonances ν5, ν6, and ν16. These experiments indicate possible chaotic motion due to overlapping resonances. A secular resonance may overlap with another secular resonance or with a mean motion resonance. The role of the secular resonances as possible sources of meteorites is discussed.
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