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Next: Restrictions
on the Scenario Up: Initial
Distributions of Binary Previous: Initial
Distributions of Binary
We have assumed a constant in time star formation rate and the total
number of stars in the Galaxy, 
, to be such that the total mass of the galaxy is 
; assuming the Salpeter mass function 
, we get
where 
stands for the minimum possible mass of the main sequence star. With 
, 
and 
, we obtain 
2.6 
stars in such a galaxy. This number agrees with a standard estimation of
the galactic star formation rate of order of 
per year. In each run of calculations, we trace the evolution of 
binaries with initial parameters randomly distributed according to the
chosen initial laws. The evolution of each binary is calculated until either
it comes to the stage where both components remain unchanged (say, double
BH or BH with NS in a wide enough orbit that the orbital evolution due
to the GR can be neglected), or until the time of evolution reaches a maximum
value, 
yr.
We calculate the total number of systems, 
, passed through a given evolutionary stage ``i'', and calculate
the sum of the stage durations, 
. Then the total number of systems 
at the given evolutionary stage simultaneously existing in the Milky Way
is estimated as
The number of the initial binaries was taken high enough (typically
1 million each run) to produce a significant statistics ( 
) for every stage of interest.