ASTRONOMY. 



139 



any known ]):ur. Tlio elements, however, iiic only to be regarded as 

 j)ro\isi()nal. 



For 85 Pegasi, Mr. Schaeberle has deduced i)roi)er motions of -f ()^833 

 ill right ascension, and — 1".005 in declination. 



Elements of hiuari/ fitars. 



Star. 



B Eiiuulei 



p Dt-lphiiii 



8.-) Pej^nisi 



5;;il21 



O .218 



70 (ji) Ojiliiuclii 

 U (J) Oiiidiis... 



y 1757 



2> Eiidaiii 



AO lihiclii 



29i8 



Tiinn of r°^^'f 



. tlOU 01 



l...r..>st.on j,^,^^ 



T 



189J. 

 18(!8. 

 3834. 

 3878. 

 1882. 

 1807. 

 1959. 

 1791. 

 1823. 

 1787. 

 1710. 



03 



8o0 



CO 



51G8 



857 



C5 



05 



98 



55 



9 







24.05 



10. 938 

 300. 1 



24. 847 

 2. 130 

 120.1 



09.0 



87. G 

 135.0 

 105.5 

 IGG. 5 



Posi- 

 tion of 

 porias- 



t ron 

 A 



2G.C1 

 2J0. 952 



70.3 

 129.454 



21.899 

 171.8 

 302.7 

 185.4 

 210.0 

 152.5 



93. G 



Iiicli- Eccon- 

 natiou tricity 



75 1 0, 

 582 0, 

 G ! 0, 

 430 0. 

 847 0. 

 0. 



Semi- 

 axis 



Mean 

 motion 



2011 

 09022 

 35 I 

 308C3I 

 58300, 

 4912 4 

 2465 

 4498 

 674 

 4424 

 229 



400 



4G000 



9G 



07254 



88349 



50 



22 



05 



90 



53 



G4 



098 

 89 

 .30 

 19 



9638 

 741 



Perioil 



year^4 

 P 



478 



955 



3 



CI88 



C53 



8( 



48 



92 



37 



5 



Computer. 



AViiiblewslvy. 



Celoiia. 



Scliaebcrle. 



Cfloria. 



Celoiia. 



Gore. 



Gore. 



Gore. 



Gore. 



Glasenapp. 



Gore. 



The imiltiple 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 +10^6 in right ascension, and to —11" in declination. 

 The close pair, A and B, 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 companion, has moved through about 55° of posi- 

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

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

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

 turbed to any appreciable extent by the iulluence of C, which is so placed 

 as not to affect their apparent relative motions, even though a very con- 

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



the most probable value of the mass of C, ^ , =2.38G, where l,w, and 

 '■ ' l-\-m ' ' ' 



m' are the masses of A, B, and 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 companion, one hitherto undetected, and 

 therefore either eniirely dark or but faintly luminous. The distance of 

 this comi)anion is probably' only a few tenths of a second, the distance of 

 C from the ])oint, Si, round Mhich 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. 



