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) gives two times worse fit with the observations, especially when accounting for galactic binary pulsar statistics (Lipunov et al., 1995f).