Документ взят из кэша поисковой машины. Адрес
оригинального документа
: http://xray.sai.msu.ru/~mystery/articles/review/node48.html
Дата изменения: Wed Feb 26 16:31:53 1997 Дата индексирования: Tue Oct 2 14:46:32 2012 Кодировка: |
Next: Artificial
Galaxy: Full Matrix Up: Restrictions
on the Scenario Previous: Binary
Pulsar Diversity and
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.