udes， we performed the following procedures. we compared the result of our main long-term integrations with some test integrations， which span much shorter periods but with much higher accuracy than the main integrations. for this purpose， we performed a much more accurate integration with a stepsize of 0.125 d (1/64 of the main integrations) spanning 3 x 105 yr， starting with the same initial conditions as in the n?1 integration. we consider that this test integration provides us with a ‘pseudo-ue’ solution of planetary orbital evolution. next， we compare the test integration with the main integration， n?1. for the period of 3 x 105 yr， we see a diffe
对火星轨道变化问题的最后解释(20/49)