KUNGL. SV. VET. AKADEMIENS HANDLINGAR. BAND 43. N:o 10. 13 
Hence 
— 
polar density 
equatorial density 3 
and consequently! 
polar axis VEN 
equatorial axis RS 
In order to investigate any inequality of distribution for the different magnitude 
classes, the gradient (variation of density) for every class is computed. This number 
exhibits a somewhat greater condensation for the fainter stars than for the brigther 
ones. According to the charts constructed by STRATONOFF,” on similar principles, 
this condensation becomes more conspicuous only from the magnitudes 7.6—38.0. 
In a following memoir [Abh. d. K. Bayerischen Akademie d. Wissenschaften 
1899], the researches of SEELIGER are continued with more particulars. The general 
assumption, according to which the stars are, on an average, equally luminous and equi- 
distant, is shown to agree very nearly with the actual distribution of stars, the stars 
up to the 
th 
n'" magnitude 
being approximately four times as numerous as the stars up to the 
n—1'" magnitude. 
A sligth discordance from this general law is, however, so far marked, as the number 
of stars from the sixth to the ninth magnitude increases somewhat more slowly than accor- 
ding to the general law just quoted. Hence the actual density of stars diminishes 
towards the boundaries of the stars” system. Furthermore the increase in number of 
stars with increasing index of magnitude proves to be greater, the nearer the considered 
region of the heavens comes to the Milky Way. 
The examination of stars up to the 11!/2 magnitude, carried out for the inter- 
val between 0” and 6” Declination by Celoria at the Milano Observatory, exhibits the 
fact that those stars behave in respect to the Milky Way in the same manner as 
the stars of the first magnitudes [1”0 to 9"0]. These Celoria-stars are of the greatest 
interest in constituting a passage from the Argelander-stars to the Herschelian stars. 
S. takes up in his researches also the last mentioned stars, comprising 683 fields of 
view, supplied with 405 fields not made known by H. and lately published by E. 
HOLDEN. According to the photometric scale these stars extend to the 13" and 14" 
magnitude. The behaviour of these stars seems to be a very different. While the 
Celoria-stars are disposed approximately in proportion to the Argelander-stars, the 
proportion of density, for the Herschelian stars, varies from 33 at the pole of the 
Galaxy to 274 in the Milky Way. The number of the faintest stars increases also in 
2 
i 
” W. SrtrAToNoFF. Publications de V'observatoire astronomique et physique de Tachkent N:o 2, 3. 
-3 
! According to HERSCHEL is 4 — 
