100 On Shooting Stars. 
x. sin. eCb 
In the same manner we obtain 6r= acts iL = 
, , ut “a 
2 = oe wt ) Also axr= sides oe ella at and it 
is evident that Bu =a, and Aw=ax cae seh with it. XBv is 
the apparent declination of the meteor seen from B, and Xv= 
R’ cos. BY. sin. (x — A’) tang. b/ 
sin. (a’ — x) t 
where the meteor stood in the zenith, and we have tang. y= 
t / 3) fe 
ee tang. b’ sin.(x 23 oe B’ sin. (a an) i tas oc 
tang. b” sin. (e — A”)-+tang. B” sin. (a” — x) 
sin. (a//— A” 
These two values of y should be exactly equal; but as the lines 
of direction are seldom given with such exactness as actually to in- 
tersect, these two values almost always differ somewhat, and this 
difference, if not too great, serves to shew the probable accuracy of 
the two observations; whereas, if the amount is considerable, it 
shews either that we have united too observations which are not cor- 
respondent, or that the observations are too loose to allow any con- 
fidence in the result. 
Finally take ¢ the distance of the meteor from the center of the 
itt wed Sade in Ce _’ cos. BY sin. hae ») 
cos. y cos. y sin. (a’ — 2) 
R” cos. B” sin. ( galt aes —A”) 
Cos. y Sin. (a” — a) 
of y, we may see how nearly correct we can regard the calculated 
height =e—R. 
The distance from the first place of observation, is Bu sec. b= 
R’ cos. B’ sin. (a — A’) R’ cos. B” sin. (e— A”) 
sin. (a’—a) cos.’ from the second =— = (a” —x cos. 0” 
A detail of the observations and the calculations for each meteor 
would probably possess little interest for most readers of the Jour- 
nal. The more important results are contained in the following ta- 
pe A few particulars respecting individual meteors are appen- 
Put y=the latitude of the place 
manner tang. y= 
; and if we here employ the two values 
