** Authors:**
S. KARAALİ

** Abstract: **
A method for the determination of the number of stars within given absolute
magnitudes with an apparent magnitude interval is presented. The relative
solar normalizations (Table 1) for Population I, Intermediate Population
II, and Population II transform Gliese's [5] total solar densities to the
solar densities for these individual populations for a given (M_{i}(G),
M_{i+1} (G)) absolute magnitude interval. The combination of these solar
densities with the corresponding model curve gives the density of the
pyramid whose height and centroid distances are r and \vec{r}
respectively, where $r$ correspods to the faintest magnitude G_{k+1} of
the interval (G_{k},G_{k+1}). The number of stars, N_{k+1} with given
absolute magnitudes and not fainter than G_{k+1} is the density of the
pyramid times its volume. Finally, if N_{k} corresponds to the apparent
magnitude G_{k}, then N=N_{k+1}-N_{k} gives the number of stars in the
interval (G_{k}, G_{k+1}) with given absolute magnitudes. The application
of the method to stars not fainter than G=16 magn. in the absolute
magnitude intervals 4

** Keywords: **