outer jovian planets. Another thing we notice is that the inner planetary subsystem may become unstable more rapidly than the outer one because of its shorter orbital time-scales. This can be seen in the panels denoted asinner 4 in Fig. 7 where the longer-periodic and irregular oscillations are more apparent than in the panels denoted astotal 9. Actually， the fluctuations in theinner 4 panels are to a large extent as a result of the orbital variation of the Mercury. However， we cannot neglect the contribution from other terrestrial planets， as we will see in subsequent sections.
4.4 Long-term coupling of several neighbouring planet pairs
Let us see some individual variations of planetary orbital energy and angular momentum expressed by the low-pass filtered Delaunay elements. Figs 10 and 11 show long-term evolution of the orbital energy of each planet and the angular momentum in N+1 and N−2 integrations. We notice that some planets form apparent pairs in terms of orbital
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