WITH A STAR OBSERVED BY I.AI.ANDE. 



151 



With these elements which are the result of ohserved motions of Leverrier, and of 

 observed residual perturbations of Hcrschcl, I have computed Levcrrier's place for May 

 10th, 1795, and reduced this place to the apparent equinox of that date, and to the actual 

 condition of Lalande's clock and quadrant. The results are, 



VI. May 10th, 1795, Leverrier as -* 7.8 mag. 14/j. 3m. 14».81 ; 59° 26' 47"; Case I. 



14 14 10 .48 ; 60 23 20 ; Case II. 



It appears at once, on comparison with these computed places, that there is no star in 

 the H. C. near the first which is not also in Bessers Zones. The second place, for Case 

 II., points at once to the remarkable star 7.8 mag., 14//. 11m. 23s.5; 60° 7' 19". 



In order to determine the quadrant reading which the computed place would have from 

 Elements II., Case II., if we vary the eccentricity so as to make the ephemeris give, for 

 Lalande's clock time, 14//. 11m. 23s.5, I subjoin the locus of Leverrier, May 10th, 1795, 

 for Case I. and Case II., and for eccentricities varying within the probable limit of that 

 clement. These limits I have taken as follows. 



Minimum limit for v =0, r = 30.005064, e = 0.006474 



Maximum limit greater than that of Jupiter, Saturn, or Uranus, e = 0.06 



The position of the missing star of Lalande for 1800 is. 



It. A. 1800 



* 7.8 mag. 14/i. 12m. 0«.9 — 1 1 ° 20 . r »H ' 

 Leverrier by interpolation, 14 12 0.(1 — 1 1 22 56 



Eccentricity by interpolation, 0.009875 



The rigorous computation does not present so close a coincidence as my firs! approx- 

 imation, February 2d. The place by interpolation is suited to the actual radius vectol 



' Value for ElcinrnN II. hum fnrmul.i \ 



