272 
PRELIMINARY GENERAL CATALOGUE OF STARS FOR 1900 
No. 3798. | Bootis c.g. 2 1888. 
The period of this binary is 148.46 years according to Biesbroeck (, 4 .Ak, 3989), and the mag¬ 
nitudes of the components are 4 M 8 and 6^7. Although the position angle of the companion had 
described less than 180° within the period of accurate measurements, the orbits recently computed 
are apparently entitled to greater weight than is usual under such circumstances. However, the 
relative motion of the components has been slowly accelerating up to the present time; and this is 
a condition that makes for uncertainty in prediction. Yet it is probably better to make some 
attempt to determine the relation of the masses of the two stars, and then refer the motion of the 
components to the resulting center of gravity than it would be to assume that the motion of either 
star is rectilinear. For the distance of the brighter star from the center of gravity, reckoned in 
terms of p, the distance between the two stars, we have: 
From right-ascension, .60 p wt. 2 
From deck, .41 p wt. 5 
Adopted, .47 p 
Accordingly, putting the mass of the brighter star as unity, that of the companion would be .87. 
If the numbers of the following table be added to the catalogue-position of the corresponding dates, 
we shall have the places of the brighter star. Multiplying the tabular numbers by —1.15, and 
adding to the catalogue-place, produces the corresponding positions of the companion. 
Date. 
Aa. 
AS. 
Date. 
Aa. 
AS. 
Date. 
Aa. 
AS. 
s 
ft 
s 
// 
s 
ft 
1824 
+ .094 
- 3- J 3 
1888 
+ .110 
+ .42 
1908 
—.028 
+ -94 
1832 
+ .114 
- 2-95 
1892 
+ .091 
+ .72 
1910 
-•043 
+ .72 
1840 
+ -I 3 1 
-2.68 
1896 
4- .068 
+ .98 
1912 
-•055 
+ -45 
1848 
+ .144 
-2.32 
1900 
+ -°39 
+ 1.15 
I 9 X 4 
—.062 
+ .14 
1856 
+ .152 
—1.89 
1902 
+ .023 
+1.18 
1916 
—.067 
- .17 
1864 
+ •154 
-1.38 
1904 
+ .006 
+1.16 
1920 
—.068 
- .78 
1872 
1880 
+ .149 
+ •135 
— .82 
— .21 
1906 
— .012 
+ 1.09 
1924 
-.036 
—1.28 
Nos. 3846 and 3847. Grw^ 1220 and Br 1923. 44 Bootis i. 2 1909. 
The positions in the Catalogue are given to the nearest o?i and 1" only because of the well- 
marked binary motion of the two components. In particular, the fact that the companion reached 
apastron about 1870 and is now well on its way toward periastron, with accelerating motion, tends 
to make future prediction unsafe, in view of the absence of knowledge as to the approximate ele¬ 
ments of the orbit. The magnitudes, about 5^2 and 6”2, do not appear to be sufficiently unequal 
to render marked inequality of masses probable. The center of gravity is likely to be near the 
mean between the two stars. Adopting the mean, we should have: 
R. A. = 15 11 o m 29?537- Deck = + 48° 2' 35V65. p- = — s o4o6. p! = -f ''028 
No. 3923. -q Coronae Bor. 2 1937. 
A very well-known binary. The period is about 41.5 years; the distances never much exceed 
1"; and the magnitudes of the two stars are assumed to be about 5^7 and 6^2. The meridian 
observers have necessarily pointed upon the general mass of light, and this can not have been very 
different from the center of gravity, to which the catalogue-position may be supposed approxi¬ 
mately to correspond. 
No. 3960. 5 Serpentis. 2 1954. 
Among the meridian-observations employed in this discussion, none previous to 1850 refer to 
the south star. If the position for 1900 of that component is desired, it can best be obtained through 
the micrometer-differences, thus: 
South star, s“i. R. A. = 15 11 30™ 1H92. Deck = + io° 52' 19''40. p = — ?oo4i. p! = —''004 
No. 3988. £ 2 Coronae Bor. 2 1965. 
The companion is of magnitude 6^1, and is very nearly fixed with reference to the principal star 
at a distance of 6". Meridian observers neglected the companion, however, until near i860. Con- 
