
 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 timedependent 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) 
