parg the variations of energy and angular ontu of the ner four plas and all ne plas， it is apparent that the aplitudes of those of the ner plas are uch saller than those of all ne plas: the aplitudes of the outer five plas are uch larr than those of the ner plas this does not an that the ner terrestrial plaary subsyste is ore stable than the outer one: this is siply a result of the relative sallness of the asses of the four terrestrial plas pared with those of the outer jovian plas another thg we notice is that the ner plaary subsyste ay bee unstable ore rapidly than the outer one becae of its shorter orbital ti-scales this can be seen the panels denoted asner 4 fig 7 where the lonr-periodic and irregular oscillations are ore apparent than the panels denoted astotal 9 actually， the fctuations thener 4 panels are to a lar extent as a result of the orbital variation of the rcury however， we cannot neglect the ntribution fro other terrestrial plas， as we will see subseent sections

44 long-ter uplg of several neighbourg pla pairs

let see dividual variations of plaary orbital energy and angular ontu expressed by the low-pass filtered delaunay elents figs 10 and 11 show long-ter evotion of the orbital energy of each pla and the angular ontu n+1 and n&;2 tegrations we notice that plas for apparent pairs ters of orbital energy and angular ontu ex插n particular， ven and earth ake a typical pair the figures， they show negative rrelations ex插n of energy and