Turkish Journal of Physics

A Method for the Determination of the Number of Stars for Different Population Types






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

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