Abstract
Following the approach taken by Bahcall and Soneira (1980) the author develops a model for the distribution of stars in our Galaxy. This model consists of three stellar components, and of one component which is intended to represent the absorption layer (dust) in the galactic plane. The model is used to predict the 2.4 μm flux observations in the interval -70 ≤ l ≤ 60 so that the values for several constants of its mathematical description could be fixed. Subsequently the model is successfully used in predicting infrared stellar counts taken from the literature for different directions in the Galaxy.
