Order of the Stanly JPirmament. 81 



it, the primary being of the sixth and the companion of 

 about the tenth magnitude^ But our telescope has proved 

 that the primary itself is a double star of the first class, com- 

 posed of two single stars of the seventh magnitude. Also 

 according to Herscli|ell as well as the observations previously 

 made at Dorpat, and those of Messrs. Herschell, the son, 

 and South, the star 4 of CassiopcE was regarded as double. 

 But our Fraunhofer has shown that the primary is composed 

 of two very proximate stars of the ninth magnitude. All 

 astronomers provided with good instruments have observed 

 a trapezium of four stars, of various brightness, in the midst 

 of the nebulae of Orion. The two Herschells, and Schroter 

 in particular, have examined this curious object. Our in- 

 strument however shows a fifth star, remarked by no prece- 

 ding observer. Mr. Herschell has since observed it with his 

 twenty feet reflector. 



Our Sun is decidedly a single fixed star. If it formed a 

 double star with some other, the latter must from its proxim- 

 ity, be distinguished from all others by its magnitude, much 

 beyond that of Sirius itself, and its change of position in the 

 heavens would characterize it still more clearly. Suppose 

 for example, that the time of its revolution was equal to that 

 of the companion of p Serpentarius, we should then observe 

 in it a movement of more than seven degrees annually, and 

 even if its revolution were a hundred times longer, its proper 

 motion must be fifty times greater than that of 6 1 of the 

 Swan, which is the most considerable hitherto observed. 



Another question which arises from the consideration of 

 this subject is, whether there does not exist between two 

 stars of the first magnitude, some mutual relation, analo- 

 gous to that of double stars, and which on account of their 

 greater proximity to us, we do not at first discover. If we 

 find any remarkable approach between stars of the first 

 magnitude, such a relation would acquire some probability. 

 Now there are in the northern hemisphere, three hundred 

 and six stars of the first to the fourth magnitude, and three 

 hundred and seventeen in the southern hemisphere, viz. 



1st 2a 3d 4th 



Northern hemisphere, 9 stars, 26, 76, 195. 



Southern do. 9, 26, 101, 181. 



The smaller number of stars of the third magnitude, in 

 the northern, being compensated by a greater number of the 

 fourth. A calculation founded on those numbers, and com- 



Vol. XV.— No. 1. 11 



