32 
intervals. At 15h. 35m. clouds came on again very sud- 
denly, and the sky remained obscured at 16h. 5m., when I 
ceased to watch. 
During the whole time of observation the sky was rarely 
entirely free from clouds for more than two or three minutes, 
but the errors arising from this cause are probably pretty 
evenly distributed through the intervals above given, and 
cannot therefore materially affect the final determination of 
the time of maximum frequency. The results of the obser- 
vations are as follows : — 
Average Number of 
Meteors per Minute. 
At 12 h 24 m 3-7 
40 9-5 
56 17-9 
13 12 23-6 
23 20-3 
34 19*7 
14 30J 2*3 
15 27J 0-4 
The curve formed by a projection of these numbers gives 
13h. 12m. as the time of maximum frequency. The probable 
error of this result can hardly exceed one minute. 
In order to determine the position of the radiant point, 
the positions of the intersecting points of the paths, con- 
tinued backwards, of a great number of pairs of meteors 
were noted. By far the greater number of these points fell 
on a space bounded by lines joining the stars y, £, /u, e, and 
Leonis, and, allowing equal weights to all the observa- 
tions, the mean position was found to be It. A. 9h. 58m. 12s. 
= 149° 33'; Dec. 22° 57*5' North. Calculating the position 
referred to the ecliptic, we have Long. = 143° 41 *0'; Lat.= 
9° 54*5' North. 
At the time of maximum frequency the earth was ad- 
vancing in the direction of a point on the ecliptic the longi- 
tude of which was 141° 28 ’3', or 2° 12 , 7 / less than that of 
the radiant. It appears, therefore, that the meteors were 
