Artificial Galaxy: Full Matrix Restrictions on the Scenario Binary Pulsar Diversity and

X-ray Galactic Sources and Binary Radiopulsars as Probes of the Initial Mass Ratio f(q) and Kick Velocity w

 

Now we present the topographical map for the COOC criterion calculated for both galactic X-ray sources taken from Table 4 and binary pulsar species from Table 6 in coordinates the initial mass ratio exponent - mean kick velocity (Figure 26). The calculations were performed for both the maxwellian (equation 7.4.1) - (left-hand panel) and Lyne and Lorimer's (equation 7.4.2)  - (right-hand panel) distributions for the kick velocity w. The innermost curve corresponds to a half-an-order uncertainty between observations and calculations (COOC = 3.3).

As we have shown just above, the binary pulsars' statistics favor lower kick velocities, whereas Galactic X-ray luminosity acts in the opposite direction. This largely defines the shape of the curves in Figure 26. A wide kick velocity distribution (like Lyne and Lorimer's) allows a wider region of parameters and w for the same comparison level between observations and calculations. If one takes Lyne and Lorimer's kick with  km s , the feasible initial mass ratio exponent can range from 0 to 1.5 within a seven times uncertainty between the observations and calculations.

 

Figure 26: The COOC criterion for X-ray galactic sources and binary radiopulsars versus the initial mass ratio exponent and mean space kick velocity for different kick velocity distributions.