第96頁(第1/4 頁)

fro that pot of view， any of the previo long-ter nurical tegrations cded only the outer five plas (ssan ≈ap; wisdo 1988; koshita ≈ap; nakai 1996) this is becae the orbital periods of the outer plas are uch lonr than those of the ner four plas that it is uch easier to follow the syste for a given tegration period at present， the lonst nurical tegrations publi射d journals are those of duncan ≈ap; lissauer (1998) although their a tart was the effect of post-a-seence lar ass loss on the stability of plaary orbits， they perford any tegrations verg up to &si;1011 yr of the orbital otions of the four jovian plas the itial orbital elents and asses of plas are the sa as those of our lar syste duncan ≈ap; lissauers paper， but they decrease the ass of the sun gradually their nurical experts this is becae they nsider the effect of post-a-seence lar ass loss the paper nseently， they found that the crossg ti-scale of plaary orbits， which can be a typical dicator of the stability ti-scale， is ite sensitive to the rate of ass decrease of the sun when the ass of the sun is close to its present vae， the jovian plas rea stable over 1010 yr， or perhaps lonr duncan ≈ap; lissauer al perford four siilar experts on the orbital otion of seven plas (ven to neptune)， which ver a span of &si;109 yr their experts on the seven plas are not yet prehensive， but it sees that the terrestrial plas al rea stable durg the tegration period， atag alost regular oscillations

on the othe