Gore — A Catalogue of Binary Stars, 8fc, 577 
6. p Eridani. About 120° of the apparent orbit has been described 
between 1825 and 1888, the distance increasing from about 2"-l to 
6"* 8. The period found by Doberck seems certainly too small. My 
orbit represents all the measures satisfactorily, and Dunlop's in 1825 
within - 5°-5. The following are some recent measures : — 
1886-901 
229°-9 : 
6" 
•63, 
Pollock. 
1886-909 , 
230 
•8 
6 
•85, 
n 
1887-121 
232 
•3 
6 
•89, Tebbutt. 
1887-131 
: 231 
•4 
. 6 
•90, 
J) 
1887-734 
: 230 
•7 
1887-747 
229 
•5 
6 
•91, 
1887-934 
228 
•5 
. 7 
•27, 
>) 
1888-038 
228 
-1 
6 
•66, 
7. Struye 228. An arc o about 130° of the apparent orbit has 
been described between 1829 and 1889. My orbit represents all the 
measures fairly well for so close a pair, the greatest difference {6o- Be) 
being + 11-27 at the epoch 1888-142 when it was measured 33*60 by 
Schiaparelli. This measure, however, does not agree with Schiaparelli's 
later measures. 
Some recent measures are : 
1888- 931 
1889- 018 
1889-021 
1889- 570 
1890- 09 
25°-73 : 0"-36, Schiaparelli. 
30 -25 : 0 •SS, 
34 ^56 : 0 -41, Young. 
26 -97 : 0 -37, Tarrant. 
41 -03 : 0 ^42, „ 
According to my orbit the distance between the components will 
gradually increase during the next few years, up to a maximum of 
about 0"-55, and then diminish again as the companion approaches 
the periastron. The minimum distance will not be reached till the 
position angle is nearly 180° (after the periastron passage), when the 
components will probably be separated by less than 0''-2." {Monthly 
Notices, R. A. S., Dec. 1889.) 
8. 40 Eridani (EC). This is the double 9th magnitude companion 
to the 4-5 magnitude star 40(0^) Eridani. Eecent measures show that 
my orbit will require revision. A physical connexion possibly exists 
between the binary pair and O'^ Eridani, as both have a common proper 
motion (4"-07 per annum in the direction of positive angle 212°-4). 
The angular motion, however, if any, is very slow. The distance is 
