APPENDIX II 
2 7 5 
No. 4376. 8 Herculis. 2 3127. 
The motion of the companion relative to the principal star is evidently rectilinear. We have the 
following expressions: 
Aa = — f 202 — *0059 (T — 1900) 
AS = — i4 ,/ 56 -f- '/i6o (T — 1900) 
Whence for 1900: 
R. A. n Decl. n' 
8 M Comp. 17 11 io m 55*233 — 1*0077 + 24 0 57' iok'39 — ''003. 
No. 4419. p Herculis. 2 2161. 
The magnitudes are 4^6 and 5^5. The early observers neglected the fainter star, so that the 
p.m. computed independently for that star would not be very accurate. The micrometric differ¬ 
ence gives: 
Aa = — 1*252 — ?ooo4 (T — 1900) 
AS = + 2" 67 + ''006 (T — 1900) 
whence for 1900: 
R. A. m Decl. pf 
5^5 Comp. 17 11 2o m 13*1709 — 10036 + 37 0 14' i8' / 32 + '.'002. 
Nos. 4556 and 4557. 95 Herculis. 2 2264. 
The position of the mean was computed with the probable errors indicated for each component. 
Then by means of the micrometrical measurements, assuming the stars relatively fixed, we have 
Aa = 0I437; AS= i"ii. From these differences the positions of the separate stars are derived. 
No. 4571. 70 Ophiuchi c.g.= Br 2271. 2 2272. 
The annual parallax may be taken as o''i5. This binary system has a period of 88.4 years 
according to See ( Stellar Systems ), whose orbit is adopted in determining the relation of the center 
of gravity of the two components, which are of magnitudes 4 M 3 and 5^8. Both stars have been well 
observed; but it seemed well to reduce the observations of the fainter star to the places of the 
brighter star by means of the differences resulting from the adopted orbit. This done, it is found 
that the proportional part of the entire distance, p (reckoning from the brighter, toward the fainter 
star), at which the center of gravity is situated is, 
from meridian-observations of R. A., .48 ± .02 
from meridian-observations of deck, .42 ± .03 
The mean, .45 p, has been adopted as the most probable result, since the result from declina¬ 
tions, though having a larger probable error, is less likely to suffer from systematic errors due to 
the proximity of the two stars. Thus the mass of the fainter star in terms of that of the brighter is 
.82. It does not seem probable, in any case, that the fainter star has a larger mass than the brighter. 
The following table gives quantities which, added to the positions computed from the catalogue- 
place of the center of gravity, will give the predicted place of the principal star. Multiplying the 
tabular numbers by —1.22, and adding as before, gives the corresponding positions of the fainter 
component. 
Date. 
Aa. 
AS. 
Date. 
Aa. 
AS. 
Date. 
Aa. 
AS. 
S 
// 
S 
// 
s 
n 
1816 
+ .Oil 
+ .81 
1856 
— .176 
+1.10 
1892 
+ .036 
- .86 
1820 
— .027 
+ 1.24 
i860 
-.171 
+ 
.87 
1896 
+ •053 
- - 5 ° 
1824 
— .061 
+ i -53 
1864 
— .161 
+ 
.60 
1900 
+ .047 
+ .16 
1828 
— .091 
+1.70 
1868 
-.147 
+ 
•33 
1904 
+ .014 
+ .76 
1832 
-.117 
+ 1.78 
1872 
— .128 
+ 
.04 
1908 
— .024 
+1.21 
1836 
-•139 
+ 1.80 
1876 
— .104 
— 
.24 
1912 
-•059 
+ 1.50 
1840 
-.154 
+ I -74 
1880 
-•°75 
— 
•52 
1916 
— .090 
+ 1.67 
1844 
— .166 
+1.64 
1884 
— .040 
— 
•75 
1920 
— .116 
+ 1.76 
1848 
1852 
-.174 
-.177 
+ 1.50 
+1.32 
1888 
— .002 
.90 
1924 
-.138 
+ 1.78 
