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| | Kollerstrom's Newton's Lunar Theory in STS@UCL |
 | | A lunar theory started with five mean motions, for the Sun, Moon, lunar node, lunar apse and aphelion, as linearly time-dependent functions moving around the ecliptic. |
 | | Finally, from the node's equated position one obtained the 'reduction', to convert longitude positions from the plane of the lunar orbit to that of the ecliptic. |
 | | The new lunar equations are the second, third, sixth and seventh, with the annual equation as the first and the Variation as the fifth. |
| www.ucl.ac.uk /sts/nk/ntn.htm (1463 words) |
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