Burnham: Measures of Proper Motion Stars 
1908.249 
.266 
.271 
A and C (7.4) 
258?42 
258.18 
258.50 
69?83 
69.81 
69.89 
1908.26 
258.37 
69.84 
A and D (12.2) 
1908.249 
29° 38 
84782 
.266 
29-35 
§ 4-44 
.383 
29.85 
84.62 
1908.30 29.53 84.63 
From five positions of AC (1876 to 1908), each on three or 
more nights, the apparent motion of the principal star is: 
o'.'oSo in 55? 5 
A continuation of the measures of AB and AD will show 
whether or not there is any motion in C. 
The proper motions by Rechenberg are: 
A o 7 o 63 in 72?4 
C 0.010 in 173.8 
6524 . 
02 269. (6.5., 
-- 7 -o) 
R. A. I3 h 
27 m 26 s Decl.+ 35 0 31' 
AB and C (9.0) 
1910.091 
33 2?38 
116772 
• 093 
332.08 
116.81 
.107 
332.30 
116.93 
1910.10 
332.25 
116.82 
C is DM (35 0 ) 2461. The earlier measures are discordant in 
distance: 
1877.46 
332^92 
114764 
in B 1 
1880.05 
332.65 
ii 6.53 
in B 1 
1880.12 
332.47 
115.04 
in B 1 
1880 
333-3 
H 4-3 
A. G. Lund. 
h 1640 is 20' distant sf. 
There is a star 
11 m, 239 0 : 4578 , but 
nebula too diffused for good measures. 
6529 . 
S 650. (8.0. 
00 
R. A.13” 
28™ 9 s Decl. 
— 12° 49' 
1909.381 
137777 
49 " 10 
10.225 
I 37-58 
49.96 
10.244 
136.72 
49.62 
10.299 
I 37-98 
49.72 
1910.04 137-51 49-60 
The change is due to the proper motion of one of the stars. 
Ristenpart 07244 in 25373 
6540 . H 1234. (7.2... 10.9) 
R. A. 13” 29 m 4 s Decl. + 39 0 24' 
1908.249 
22°4 
32753 
8.266 
22.0 
32.62 
9.263 
22.6 
32.24 
1908.59 
22.3 
32.46 
The large star is Groombridge 2013 which is given a proper 
motion 0^040 in 351 78 . No early measures. 
6558 . 81 Virginis. 2 1763. ( 7-5 - * -7 - 5 ) 
R. A. i3 h 3i m 1S 3 Decl. —7° 16' 
A and C (11.4) 
1912.312 
327753 
i 40"93 
-351 
327-63 
140.92 
• 353 
327-73 
141.24 
1912.34 
327.63 
141-03 
No change in AB. The proper motion of 81 Virginis, if 
any, is so far uncertain. 
Auwers o 7 o 6 i in 228?2 
Boss 0.019 in 248.6 
6571 . 2 1769. (7-3-.-9-7) 
R. A. I3 h 32 m 50 3 Decl. + 39 0 47' 
6528 . 
(3 114. (7.6.. 
.8.0) 
R. A.13” 
28™ o 3 Decl. 
— 8° 0' 
1908.252 
i 4 i 79 
1748 
.2 66 
142.1 
i -45 
1908.26 
142.0 
1.46 
This pair was observed by Glaisher at the Cambridge Ob¬ 
servatory in 1842 who used it for comparison with Mars. 
These measures are of special interest as confirming the slow 
direct motion shown by the later observations. 
1842.33 12678 1^38 2n 
The three 2 stars appear to have a common proper motion 
of about 0^25, and to verify this, I have connected a third star 
with A and C. 
A and D (11.3) 
1909.170 194780 168741 
.244 195-45 168.55 
.263 195-05 168.15 
1909.23 I95-io 168.37 
C and D (8.2.. .11.3) 
1909.170 175-40 152^07 
.244 175-88 152.26 
.263 175-72 152.16 
1909.23 I 75-67 152-16 
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