961 



to magnitude, giving to tlie separate results the weights of the last 

 column which I determined by a rough estimation. 



A comparison of the results for Ap in the three magnitude-groups 

 shows that the influence of magnitude on the precession-correction 

 is not perceptible, while it remains uncertain whether there is a 

 systematic difference between the results deduced from R.A. and 

 Decl. ; it is certainly not great. The exclusion of a single result has 

 immediately a great influence upon the final value. Taking everything 

 together there would seem to follow as final result: 



Lp = -j- 0"25 per century, 



whereby the precession constants for 1850 would become: 



jt^i = lunisolar-precession = 50"3709 



m = precession in R.A. ==46.0734 



71 = precession in Decl. = 20.0521. 



6. Results for the elements of the solar motion. 



The results of the ^-solutions have no sharply defined significance 

 for the value of the solar motion. I therefore combined in the 

 following table the results of the groups ^' and ^ of the comparison 

 Kü — B.Z. ; I also included in the results the ^-solutions of the 

 differences Kü — A. G. -catalogues. The values are throughout the 

 mean of three results, obtained according to the systems of Auwers, 

 Newcomb, and Boss. 



Results for the solar motion. 



For the coordinates of the apex the ^-solutions may also be af 

 value. Their results are as follows: 



