This comparison shows the most inclined orbits to be also very eccentric; Bertha and Eunice being the only exceptions in the foregoing list. On the other hand, however, we find over fifty asteroids with eccentricities exceeding 0.20 whose inclinations are not extraordinary. The dependence of the phenomena on a common cause can, therefore, hardly be admitted. At least, the forces which produced the great eccentricity failed in a majority of cases to cause high inclinations. 8. Longitudes of the Perihelia. The perihelia of the asteroidal orbits are very unequally distributed; one hundred and thirty-six--a majority of the whole number determined--being within the 120° from longitude 290° 50´ to 59° 50´. The maximum occurs between 30° and 60°, where thirty-five perihelia are found in 30° of longitude. 9. Distribution of the Ascending Nodes. An inspection of the column containing the longitudes of the ascending nodes, in Table II., indicates two well-marked maxima, each extending about sixty degrees, in opposite parts of the heavens. I. From 310° to 10°, containing 61 ascending nodes. II. " 120° to 180°, " 59 " " --- Making in 120° 120 " " A uniform distribution would give 89. An arc of 84°--from 46° to 130°--contains the ascending nodes of all the old planets. This arc, it will be noticed, is not coincident with either of the maxima found for the asteroids. 10. The Periods. Since, according to Kepler's third law, the periods of planets depend upon their mean distances, the clustering tendency found in the latter must obtain also in the former. This marked irregularity in the order of periods is seen below. Between 1100 and 1200 days 6 periods. " 1200 " 1300 " 7 " " 1300 " 1400 " 43 " " 1400 " 1500 " 13 " " 1500 " 1600 " 46 " " 1600 " 1700 " 54 " " 1700 " 1800 " 20 " " 1800 " 1900 " 13 " " 1900 " 2000 " 19 " " 2000 " 2100 " 33 " " 2100 " 2200 " 2 " " 2200 " 2300 " 2 " " 2300 " 2400 " 8 " " 2400 " 2800 " 0 " " 2800 " 2900 " 2 "