(373) 
which equations are identical with (15) if we introduce in them the 
same suppositions. 
So, here again we find, that zones of identical À, will Icad to 
approximately the same results in the two methods. What hoids 
for each of the zones separately, must also hold with some approx- 
imation for the final results. 
For Kosotp’s method the approximation will be sornewhat less 
satisfactory. For here we must neglect terms of the order 
paA, pdD, p* 
to gain our end. 
If we do this, the equations (36) will become 
2 sin? À, (ea Jaa + 2 sin? À, ee 4 dD = — 2 sin? i, ap 2 
2 sin® A, a a dA + 2 sin? À ty |ap= — 2 sin? A [twp 2) 
which are again identical with our equations (15) if we introduce 
in them the same suppositions. Zones of identical À treated according 
to both methods giving approximately identical results, this must 
lead here also to pretty nearly the same final results. 
The calculations of KosorLp (Astr. Nachr. N°. 3592) confirm this 
conclusion. ‘The solution which he makes with mean proper motions 
is the only one which is in a somewhat tolerable agreement with 
what others have found, calculating with other methods but also 
with mean values of the proper motions. 
Kosotp finds A = 262°.8 D= + 16°.5 
L. Srruve finds A= 2738°.3 D= + 27°.3 
After all that has been said the conclusion is pretty obvious 
that what, perhaps more than anything else, must hinder us in 
accepting the methods used until now for the derivation ot the 
direction of the solar motion is this: that quantities are treated as 
small ones, which in reality are not small }). 
1) From an utterance of Prof. Newcoms [ conclude that he too ascribes the deviating 
result of Kosotp to the reason here stated. 
