Next: The Effect of Kick Up: Restrictions on the Scenario Previous: Test of the Initial
Next: The
Effect of Kick Up: Restrictions
on the Scenario Previous: Test
of the Initial
Now we turn to the discussion of the influence of the kick velocity
imparted to NS at birth. The formation of a NS during a supernova explosion
is usually accompanied by a catastrophic mass loss,
which in the majority of cases leads to disruption of the binary system;
a young NS can thus "remember" the orbital velocity of the progenitor
star of the order of a few 100 km s
before the collapse (``Blaauw mechanism'', Blaauw,
1955[17]; Gott et al., 1970[57]).
However, the range of stellar parameters (masses, radii, orbital separations,
etc.) is so wide that some of the systems must survive as binaries during
the cataclysmic processes of stellar collapse (see Bhattacharia and van
den Heuvel, 1991[12]). Thus,
the standard scenario of binary system evolution naturally produces diverse
species of pulsars, on the one hand, and explains the velocities of radiopulsars
of about 100-200 km s
measured shortly after their discovery (Manchester and Taylor, 1977[133]),
on the other hand.
Recently reported new measurements of the radiopulsars' proper motion
(Lyne and Lorrimer, 1994[132])
and of young pulsar positions inside the associated supernova remnants
(Frail et al., 1994[53])
imply much higher birth velocities of 
500-900 km s
for pulsars than follows from the standard scenario. This revives the idea
of an asymmetrical supernova collapse which was put
forward for the first time by I.S. Shklovskii (1970)[179].
Owing to an enormous energy liberated during the collapse, which is comparable
to the rest-mass energy of the whole star, 
, a small anisotropy 
would be sufficient for the remnant to leave the Galaxy, 
, where c is the speed of light. A number
of anisotropy mechanisms have been proposed: asymmetric neutrino emission
in a strong magnetic field during collapse (Chugai, 1984[32],
Bisnovatyi-Kogan, 1993[14]); double NS
formation during core collapse (Imshennik, 1992[77]);
tidally induced asymmetric ignition of the WD during the AIC (Lipunov,
1983[103], Lipunov et al., 1987b[121])
etc. However, a reliable reason for such anisotropy still remains unclear.
Thus, as for the cosmological constant term, the anisotropy was released
away (like a jinnee from the bottle) as a possible but not necessary thing.
It seems natural to assume that the kick velocity is arbitrarily directed
in space. The value of the kick velocity w
can be quite different and may well depend on a number of parameters, such
as magnetic field strength, angular velocity and so on; we consider two
extreme assumptions of a strongly determined distribution, 
and of a maxwellian-like one,
which is natural to expect if several independent approximately equally
powerful anisotropy mechanisms operates randomly. Here 
is a parameter which is connected with the mean kick velocity 
by the relation 
.
In addition, we performed calculations for the kick velocity distribution taken so as to fit the observed transverse pulsars' velocity obtained by Lyne and Lorimer (1994)[132]:
where 
,
is a parameter. The best-fit to Lyne and Lorimer's two-dimensional distribution
is reached at 
km s
.
