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Basic Observational Data for Determination of f(q) and tex2html_wrap_inline8879

The numbers of binary systems at different evolutionary stages are most sensitive to f(q), w and tex2html_wrap_inline8879 , 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) tex2html_wrap_inline8845 (number of sources) tex2html_wrap_inline10436 (average stage duration) tex2html_wrap_inline10438 and thus is independent of the poorly known values of accretion rate tex2html_wrap_inline9166 and accretion stage duration tex2html_wrap_inline10442 .


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.


Mike E. Prokhorov
Sat Feb 22 18:38:13 MSK 1997