Table 2
Secular representation of the Earth orbital dynamics given by the Lagrange-Laplace theory.
| μi | Ei | max[Ei] |
|---|---|---|
| (″ yr−1) | (×105) | (×105) |
| 3.7137 | 1628 | 1974 |
| 18.0043 | 1492 | 1917 |
| 7.3460 | 1490 | 3286 |
| 17.3308 | 1057 | 2381 |
| 5.4615 | 404 | 600 |
| 22.2944 | 247 | 385 |
| 2.7015 | 61 | 194 |
| 0.6333 | 1 | 2 |
| νi | Si | max[Si] |
| (″ yr−1) | (×105) | (×105) |
| 0.0000 | 1377 | 2420 |
| −18.7456 | 1222 | 1989 |
| −6.5701 | 409 | 3424 |
| −5.2008 | 425 | 1606 |
| −17.6358 | 226 | 929 |
| −25.7514 | 141 | 733 |
| −2.9039 | 87 | 993 |
| −0.6778 | 65 | 895 |
Notes. The eight planets of the Solar System are included. In the third column, each amplitude is maximised in the case where both the mutual inclinations and the longitudes are unknown, assuming the equipartition of AMD between secular degrees of freedom (since the Solar System is hierarchically AMD stable, the AMD of the inner and outer parts were taken separately, see Laskar & Petit 2017). The initial conditions and physical parameters are taken from Bretagnon (1982).
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