|
Документ взят из кэша поисковой машины. Адрес
оригинального документа
: http://xray.sai.msu.ru/~lipunov/kionewht/node9.html
Дата изменения: Fri Jun 16 18:37:02 2000 Дата индексирования: Tue Oct 2 02:58:11 2012 Кодировка: Поисковые слова: о п р п |
To calculate binary evolution, we have used the population synthesis method (the Scenario Machine code), which is in fact a version of the Monte-Carlo calculations. Here we shall not enter into detail of the evolutionary scenario used. Much more detailed description of the method can be found in our review [16].
Figure: Massive binary evolutionary track.
An example of the evolutionary track leading to BH+BH binary system
formation is shown in Fig.
. A short glance to this track
is sufficient to understand that there are a lot of evolutionary
scenario parameters, which affect different stages of the binary
evolution. Fortunately, a very limited number of parameters has effect
on the compact binary merging rate.
Kick
The most important (and practically unique) parameter changing the galactic binary NS merging rate is the distribution of an additional (kick) velocity imparted to NS at birth. The kick velocity distribution widely accepted at present is derived from the analysis of spatial velocities of single radiopulsars [17].
We have approximated this 3-dimensional distribution as
where 
and the characteristic velocity
is a parameter in our calculations. The observed
pulsar transverse velocity distribution corresponds to
km/s.
Critical Mass and Collapse Mass Fraction
In contrast, for BH two additional parameters appear.
First of them is a threshold main sequence stellar mass
for the star to collapse into a BH after
its nuclear evolution has ended.
This parameter is still poorly
determined and varies in a wide range:
e.g., according to van den Heuvel and Habets
[18] 
-80M 
;
Tsujimoto et al. [19] give 40-60M ; Portegies Zwart
et al. [20] derive >20M .
The second parameter is the fraction of the presupernova mass,
, collapsing into BH. This parameter is fully unknown, so
we varied it from 0.1 to 1 in our calculations.
The third parameter, as for NS, is the kick velocity. Clearly, in the general case the more massive BH will acquire smaller velocities than NS. In our calculation we used the following ad hoc relationship
where 
M is the maximal NS mass
(Oppenheimer-Volkoff limit). When BH mass is close to
, velocities of BH and NS are assumed to be almost the same,
whereas at 
BH kick velocity is assumed to vanish.
(Of course, other dependences 
are possible, but
their specific shape weakly affects the results).