172 
W. Beebe — The Comet of 1771. 
C-0 
Aa 
A3 
June 1, 
- 37-7 
+ 1 37 
9, 
- 8-1 
- 1 33 
25, 
+ 46-6 
+ 51 
July 11, 
-2 8-5 
4- 57 
Comparing these results with those of Encke we find a close agree- 
ment, especially in the most probable eccentricity. The increase in 
the residuals on passing to the most probable parabola is also about 
the same. 
II. 
In computing the perturbations, the action of Venus was not con- 
sidered. For during the whole period of observation, when alone the 
action of Venus could be sensible, the motion of the comet was just 
sufficient to keep it very close to opposition to that planet. In such 
a position the entire influence of a planet would be expressed by an 
increase in the value of k, the constant of solar attraction wherever 
used in calculating the orbit. For Venus, the value of log k would be 
unchanged to the 8th decimal place. 
The nearest approach of the comet to Mars was •35R, June 17th, 
1771, to Jupiter, about 4R, nearly a year before perihelion; and to 
Saturn, 8R, shortly after perihelion. The perturbations of the rec- 
tangular coordinates referred to the ecliptic were computed in units 
of the 7th decimal place; for Mars, at intervals of 8 days from April 
1, 1771, for Jupiter, at intervals of 20 days from July 20, 1769; and 
for Saturn, at intervals of 40 days from Jan. 1, 1770, as follows: 
$ 
dx 
dy 
dz 
April 30, 
- 1-2 
— '5 
+ 'I 
May 16, 
4-8 
- -8 
1-6 
June 1, 
13-1 
+ ‘8 
7-7 
n, 
32-4 
11-8 
24-1 
July 3, 
53-4 
392 
52T 
19, 
-68-9 
+ 77-4 
4-88-4 
U dx 
dy 
dz 
da 
dS 
April 2, —2648* 
+ 5122- 
+ 731 * 
+ 
66"*9 + 
27-6 
12, 1996 
5310 
783 
64-0 
20-8 
22, 1313 
5888 
902 
5 1 '6 
12-2 
May 2, 909 
7101 
1153 
+ 
31-9 
6-0 
12, 721 
8563 
1481 
0 
5-7 
22, 1070 
10060 
1862 
— 
33-0 
13-8 
June 1, 1687 
11632 
2278 
61*3 
30-0 
