COM M E N' T A t I A S T R N M I C A. S33 



■8. ) I/yrae «. 



« Summer zenith-distance, Jan. 1, 1811. 



1808 — 1813 65 observ. 14° 46' 19",35 + 0,18 p 



1814 20 19. 87 + 0,78;» 



1815 20 19, 86 + 0,74;j 



1816 11 20,46+0,77/» 



1817 12 19, 62 + 0,62p 



« Winter zenith-distance, hm. l, 1811. 



1808 — 1813 61 obsery. 14° 46' 20",96 — 0,79/> 



1814 — 1815 20 21,00 — 0,78/» 



1815—1816 14 19,47 — 0,68/» 



1816 - 1817 15 20, 88 — 0,76/? 



1817—1818 24 20,06 — 0,76/? 



14° 46' 19",63 4- 0,76/? = 14° 46' 20",64 — C,77/? 



«nde: p = 0",66 2p = 1",32 ex 262 observationibus. 



4. ) Draconis y. 

 53 observationes byemales dant dist. zenith. Jan. 1. 1814 ... 1° 52 17",55 

 59 « aestivae « « « « • • • 17, 92 



quod paraüasi repugnat. 



Deinde Brinkleius haec afierl ; 



« It is by Observation alone , that the decision can be made. No conjeclure as to tht 

 « relative distances of the stars can be of any malerial -weight. The conjeclure, in it- 

 « seif probable , that the brightest stars are nearest to us, seems opposed by anolher 

 « conjeclure , also by ilself probable , that ihose stars are nearest which haTC the grea. 

 « lest proper motion. " 



« Some of the brightest fixed stars have scarcely any sensible proper motions , white 

 « those of some much smallcr are very perceplible. The two stars, 61 Cygni, have 

 « eaeh an annual proper motion of about 5",3 in right ascensioh, and of 3" in decli- 

 « nation. These slars are of about the 6* magnitüde , and one a little brighter thati 

 « the olher. " 



« This great proper motion seemed to render it probable, that Ihese stars are suffi- 

 « ciently near to us , to have a visible parallax. I accordingly made observations oa 

 « one of thcm , but found nolhing satisfaclory. " ■ 



« Also 40 Eridani which is of Ihe 5* magnitude , has so great a proper motion , that 

 ■M we might conjecture it to be nearer to us than many of the brighter stars. " 



Gg € The 



