472 UNIVERSITY OF VIKGINTA PUBLICATIONS 



meteors, etc., are the principal causes for the inclusion of a radiant in this 

 table. 



Table V. — This table contains 10 orbits which seem certainly to belong 

 to the main Perseid stream. They fully confirm the connection of these 

 meteors with comet 1862 III, or Tuttle's Comet. 



Table VI. — This table contains 7 orbits which resemble each other 

 sufficiently and whose basic radiants show an approximately increasing 

 longitude, from date to date, to permit their being placed together. It is 

 believed that to the unprejudiced reader there can no longer be any doubt 

 about the fact that the Orionid radiant does slowly shift its position, as 

 this table shows. As this group of meteors has been held up as the typical 

 example of stationary radiants, the results here given are quite instructive. 

 This opportunity is taken to again point out the very close resemblance 

 of the elements of these Orionids and the ?? Aquarids.' 



Table VII. — This contains 6 orbits of the Leonid Meteors. On the 

 two dates in 1912, for both A. P. C. C. and C. P. 0., there can be no doubt 

 that two distinct radiants are shown on the maps of each. No possible 

 errors of observation could get all the meteors observed to conform to one 

 radiant for either observer. Hence the resulting orbits have been divided 

 into two groups: Leonids (1) the main stream, and Leonids (2) a sub- 

 stream which was clearly shown in 1912 on November 14. Of course the 

 elements confirm the well-lcnown connection of these meteors with Temple's 

 Comet— 1866 I. 



Table VIII. — This table shows the magnitudes of the meteors seen, as 

 observed by those of the members who sent in the larger lists. 



Table IX. — The percentages of meteors of a given magnitude to the 

 totals seen are here given for the two observers who have sufficiently large 

 numbers of observations to make these data useful. 



Table X. — The first part of this table gives the number of meteors 

 of a given color and duration. The second part gives the number of 

 meteors of a given magnitude and duration, but whose colors were not 

 recorded. As is to be expected few bright meteors come iiito the second 

 part, and of course few very faint meteors were included in the first part 

 of this table. Again the colors of red, j^ellow and orange meteors are more 

 easily detected than green or white. Hence the latter part of the table is 

 mostly made up of these last. Besides if a meteor was white, i.e., had no 

 detectable color, it was seldom recorded in the color column at all, which 

 explains why so few white meteors appear. These results are based on the 



' See Transactions of American Philosophical Society, vol. xxii., p. 11. 



