184 G. H. KNIBBS. 



There was no definite indication of a general rotation, such as 

 was symbolically represented in the form of the equations of 

 motion. 



(88) Boss, 1890.— Using stars in the Albany zone, D. = 0°50' 

 to 5 ,o 10', Boss in 1890 deduced the following results by adopting 

 Airy's method '} 



Series. 



No. of 

 Stars. 



Mag. 



R.A. 



D. 



R. 



1 



135 



6-6 



280-4 



+ 42 ? 8 



(A 239 



2 



144 



8-6 



285-7 



45-1 



0-1373 



Both 



279? 



7-6 



283-3 



44-1 2 



01309 



55 



253 



7-7 



288-7 



51-5 





Quoting Struve's, and Bischof s, and pointing out that the general 



result was about 



R.A. = 287° and D. = +47° 



Boss seemed to think that the most probable position was 



R.A. = 280°, D.= +40° 



He pointed out that Struve's result reduced on the system of the 



American Ephemeris would change its declination from +27 ,0 3 



to +37°7. 



(89) Hecker, 1891. — Hecker in 1891 by developing the observed 

 motion of a star as a function of its position and distance, and by 

 so determining the point that the motion in both coordinates 

 vanishes, obtained the values : 3 



Division I. R.A. = 272-°5, D.= +13'°8 

 „ II. 267-8 4-7 



or combining the results 



R.A. = 270°0, D. + 9-°9. 



(90) Monck, 1892. — Pointing out that although there is a con- 

 siderable amount of agreement, in the determinations of the solar 

 motion in space, the discrepancies are such as to indicate the pre- 

 carious nature, and indeed even the inadmissibility of some of the 



1 A determination of the Solar Motion. — Astr. Journ., Vol. ix., pp. 161 

 - 165, 1890. See also, The Observatory, Vol. xiii., pp. 217, 218. 



3 Newcomb corrects this afterwards to 42*°9. 



3 Ueber die Darstellung der Eigenbewegungen der Fixsterne und die 

 Bewegung des Sonnensystems. — Munchen, 1891. 



