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The numbers of binary systems at different evolutionary stages are most sensitive to f(q), w and , so the comparison with observational data can pose some restrictions to these parameters. As basic observational stages to be compared with calculations, we have chosen the objects listed in Table 4. It is important to note that we use the total accretion X-ray luminosity for low-mass X-ray binaries and not their total number, since the total accretion luminosity in the Galaxy = (average luminosity of the individual sources) (number of sources) (average stage duration) and thus is independent of the poorly known values of accretion rate and accretion stage duration .
As an example, in Table 5 we show an evolutionary track leading to the formation of typical LMXB. Brief comments on the track are also given.