194 G. H. KNIBBS. 



that of Bessel. (c) The Besselian method proceeds upon the 

 assumption that positive and negative departures from the paral- 

 lactic motion (due to the sun's motion) are equally probable. This 

 last method gives a point in the Milky Way 



R.A. = 266-°5, D.= -3-°l 

 and is of course the result previously given in 1894. 



(103) Kapteyn, 1895 (May). — In 1895 Kapteyn continued the 

 publication of his researches on the distribution of the velocities 

 of the stars in space, 1 taking account of their spectral type; the 

 general result of such researches is given hereinafter, see Kapteyn 

 1898. 



(104) Anding, 1895. — In his Habilitationschrift of about 1895 

 Anding 2 discussed the relations between the methods of Bessel 

 and Argelander for the determination of the apex of the solar 

 motion, having special reference to Kobold's work. For Kobold's 

 reply see August 1895. 



(105) Kobold, 1895 (Aug.) — Kobold having examined the 

 deductions of Anding, replied that the consequences reached by 

 his mathematical analysis were inconsistent with the actually 

 observed distribution of proper motions, and his hypothesis could 

 not be established. 3 A connection between the distribution of 

 the stars and the position of the apex of motion was certainly 

 most apparent, but it was admittedly difficult to distinguish 

 whether the actual distribution was the consequence or the cause 

 of the position of the apex-point. 



(106) Bompas, 1896 (Jan. and Mar.) — A brief discussion on a 

 possible explanation of the difference between the positions of the 

 apex of solar motion, when deduced from stars of different distances, 



1 Over de verdeeling der kosmische snelheden.— Verslagen der Afd. 

 Natuurk. Kon. Akad. v. Wetenschappen, Dl 4, 25 Mei 1895 - Apr. 1896, 

 pp. 4-18. 



2 Beziehungen zwischen den Methoden von Bessel und Argelander zur 

 Bestimmung des Sonnenapex. — Habilitationschrift, 1895. 



3 Ueber die Vertheilung der Sterne mit merklicher Eigenbewegung. — 

 JLstr. Nach., Bd. cxxxix., pp. 65 - 78. 



