Next: Basic Observational Data for Up: No Title Previous: Star Formation Rate and
Next: Basic
Observational Data for Up: No
Title Previous: Star
Formation Rate and
In this section we show that the comparison between the calculated and
observed numbers of the most ``fragile'' (from the point of view of the
binary evolution scenario) galactic binary types (such
as X-ray low-mass X-ray binaries (LMXB), cataclysmic variables (CV),
Be-stars with compact companions, relative number of
visible binary radiopulsars with normal and compact
secondary components) impose certain constraints on the feasible initial
binary mass ratio distribution chosen in a power-law form 
(see previous section). We show that the efficiency of removal of binary
angular momentum during the CE stage is much less restricted, allowing
a wide range 
-10. We specially study how different values of the kick velocity
imparted to a newborn NS taken from the range 0-1000 km s
change the results. We obtain that the kick velocity
of about 
200 km s
would fit the existing data on relative numbers of binary radiopulsars
with normal and compact companions within a half-order of magnitude uncertainty.
The high mean kick velocity of
450 km s
which appears to follow from recent radiopulsar measurements by Lyne and
Lorimer (1994)[132]
gives two times worse fit with the observations, especially when accounting
for galactic binary pulsar statistics (Lipunov et al., 1995f[130]).
