Burnham: Measures of Proper Motion Stars 
We have the following micrometer positions of AB : 
1851.18 
33°73 
204 "i 5 
in 
02 
1861.27 
34-57 
205.32 
in 
02 
1870.30 
34-97 
205.92 
in 
02 
1881.29 
35-65 
207.62 
in 
02 
1886.34 
36.05 
208.05 
2n 
Eng 
1908.10 
37.21 
210.25 
3 n 
3 
These positions give for the most probable motion of A: 
o"244 in 279?1 
Therefore the proper motion of the large star in declination 
is: 
Measures — 0^425 
Porter 0.427 
Auwers 0.432 
Boss 0.441 
Lalande 19627 (8.8...9.4) 
R. A. 9 h 59 m 9 s Decl. + 69° 2' 
The measures of BC given above when compared with Struve 
in 1830, show a slow relative motion which is undoubtedly real. 
As the smaller component of 2 1342 is only 11 m, it is safe to 
assume that the proper motion is in the other star. This 
motion is therefore: 
o"o25 in 24?o 
Applying this correction to the apparent motion of 40 Lyncis, 
we have for the real proper motion of that star: 
0^238 in 285^0 
From meridian observations this has been given: 
Stumpe 
O"250 
in 
2 76°. 7 
Auwers 
0.239 
in 
276.3 
Newcomb 
0.219 
in 
273.1 
Boss 
0.217 
in 
272.6 
aj) Leonis 
( 5 - 6 .. 
.10.9) 
R. A. 9 h 37 m 12 
8 Decl. + 14 0 34 ' 
1909.071 
! 37-97 
281"76 
.112 
138.13 
282.08 
.186 
138.08 
281.71 
1909.12 
138.06 
281.85 
1907.810 
255-25 
l8 3 "2 4 
8.079 
255-33 
183.27 
8.082 
255-25 
183.08 
1907.99 
255-28 
183.20 
The only other measures are: 
1893.25 255?33 186'.'78 2n Eng 
Giving for the motion of A : 
o"243 in 257?9 
As these stars differ but little in brightness, it is uncertain 
whether or not the motion is all in the larger. 
The results from meridian positions are discordant. 
Stumpe o"4ii in 2i9?5 
Porter 0.303 in 237.0 
To determine hereafter whether there is any motion in B, I 
have connected a third star: 
B and C (12.0) 
1912, 
.066 
325-40 
198!'09 
. 162 
325-50 
198.16 
.164 
325 -I 3 
197-49 
1912 
-13 
325-34 
197.91 
A and B are DM (69°) 558 and 557. 
All single distances. The only other measure is the fol¬ 
lowing: 
1880.17 I39°63 28o" 26 3n p 3 
The distance between the two stars is too large for the most 
accurate measures with the micrometer. These observations 
imply a larger proper motion of the large star than that found 
by meridian positions. 
Auwers 
o"oi3 
in 
261 ?3 
Newcomb 
0.030 
in 
252.2 
Boss 
0.014 
in 
I 9 I -7 
Groombridge 1618 ( 6 . 7 ... 8 . 8 ) 
R. A. 1 o'* 4 m o s Decl. + 50° 4' 
1908.025 I9i°58 172^41 
.102 191.23 172.37 
.118 191.38 172.09 
The only measured positions are: 
1894.37 I 96?45 i 83"27 2n 
1908.08 191.40 172.29 3n 
From these positions the proper motion of A is: 
P'393 in 248? 9 
Eng 
3 
This motion is larger by the meridian observations: 
20 Leortis Min (5-6...8.8) 
R. A. 9 h 54 m 6 s Decl. + 32 0 31' 
There is no comparison star near enough for direct measure¬ 
ment with the micrometer. Otto Struve compared it in R. A. 
and Decl. with DM (52 0 ) 1968, which is about 33 s following. 
The several results 
are: 
1852.19 
A Decl. — 31T92 
in 
02 
1873.27 
— 23.96 
in 
02 
1909.16 
— 9-24 
3 n 
3 
Groombridge 1*450 in 249?2 
Porter 1-447 in 249.8 
Kustner 1-459 in 249.4 
The smaller star is DM (50°) 1724. Comparing this with 
(50°) 1723, a star 9.3 m, seems to show that the former has no 
sensible motion, and that the motion of the large star, as given 
by the measures is correct, if there is no unusual error in the 
micrometer measures. 
1724 and 1723 
1908.12 254?o 303"65 in 3 
i 877-3 254.0 303.4 A. G. Harv. 
37 
