ASTRONOMY. 



139 



:uiy known i);iir. The elements, however, nie only to be regarded as 

 ])r()visioiial. 



For 8.> Pegasi, Mr. Schaeberle has deduced propei- motions of -|-(R8o3 

 in right ascension, and — 1".0()5 in declination. 



Eleinods of hinarji .slnr>^. 



Star. 



S Eciuulci 



p Di-lpljiui 



85 Pe^rasi 



X;il21 



o :2:'8 



70 (/)) Ojiliiuclii 



It (0 ()i ioui-i 



i;]757 



p Ei idaiii 



AO liiiulii 



S948 



Time of 



lieiiasl.ron 



T 



1892.03 



1808. S-W 



18S4. 00 



1878.5198 



1882.857 



1807. G5 



10.->9.05 



1791.98 



1823.55 



17S7. 9 



1710.0 



Posi- 

 tion of 

 iiodo, 



a 



24.05 



10. 9:i8 

 :-;0G. 1 



21.817 

 2. i:!0 

 120. i 



99. C 



87. G 

 135.0 

 105. 5 

 IGG. 5 



Posi- 



tiou of 



liorias- 



triiii 



2G. Gl 

 2:0. 952 



70.3 

 129.454 



21.899 

 171.8 

 ;!02. 7 

 185.4 

 210.0 

 152.* 



93. G 



Iiicli 

 nation 



Senn- 



0.2011 

 0. 09G22 

 0.35 

 0. 30803 

 0. 58300 

 0.4912 

 0. 2465 

 0. 4498 

 0.674 

 0.4424 

 0.229 



0.40G 

 0. 40000 

 0. 90 

 0. G7254 



0. 88349 

 4.50 



1. 22 

 2.05 

 G.9C 

 1.53 

 1. C4 



-4.098 

 -1.89 

 + 1.30 

 -1.19 

 + 0.9G3S 

 -0.741 



Poiioil 



yeai'.s 

 P 



478 



955 



3 



GI88 



053 



81 



48 



92 



37 



5 



Cominiter. 



AViubli'Wsliy. 



C(!loiia. 



Schaeberle. 



Ccloria. 



Celoria. 



Gore. 



Gore. 



Gore. 



Gore. 



Glaseuapp. 



Goro. 



The nniltiple star C Cancri. — Professor Seeliger's recent investigations 

 have confirmed the results of his earlier work, and those obtained by 

 Struve In 1874. "The three stars A, B, and C have the magnitudes re- 

 spectively, 5.0, 5.7, and 5.3. The proper motion of the system amounts 

 in a century to +10'*.G in right ascension, and to —11" in declination. 

 The close pair, A and P, have a motion round each other in about sixty 

 years; their apparent distance varying from about 0".G to I'M ; whilst 

 C, the more distant comi)anion, has moved through about 55° of posi- 

 tion angle round the other two since Ilerschel's observations in 1781, 

 its distance never very greatly varying from 5h". The motion of A 

 and P> round their common center of gravity does not appear to be dis- 

 turbed to any apjneciable extent by the influence of C, which is so placed 

 as not to affect their api)arent relative motions, (;ven though a very con- 

 siderable mass be assigned to it, and as a fact Professor Seeliger finds, for 



111' 

 the most probable value of the mass of C, ,_,- =2.386, where l,w, and 



m' are the masses of A, B, and C respectively. But there is a periodi- 

 cal retrogression of C itself which is most easily accounted for by sup- 

 posing the presence of a close conii)anion, one hitherto undetected, and 

 tlierefore either entirely dark or but faintly luminous. The distance of 

 this companion is probably only a few tenths of a second, the distance of 

 C from the i)oint, s-z, round which it appears to revolve, and which may 

 reasonably be assumed to be the center of gravity of itself and of I^, the 

 as yet undiscovered fourth member of the family, being only about one- 

 fifth of a second. The entire group may then be considered as a double 

 double. 



