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Next: Effect
of the Magnetic Up: ``Ecology''
of Magnetic Rotators Previous: The
Stopping Radius
The estimates presented above for the stopping radius were obtained under the assumption that the energy released during accretion does not exceed the Eddington limit, so we neglected the reverse action of radiation on the accretion flux parameters.
Now, we turn to the situation where one cannot neglect the radiation pressure. Consider this effect after Lipunov (1982b)[99]. Suppose that the accretion rate of matter captured by the magnetic rotator is such that the luminosity at the stopping radius exceeds the Eddington limit
We shall assume (after Shakura and Sunyaev, 1973)[177] that the radiation sweeps away exactly that amount of matter which is needed for the accretion luminosity of the remaining flux to be of the order of the Eddington luminosity at any radius:
This gives
where 
is a spherization radius (where the accretion luminosity
first reaches the Eddington limit), and 
designates the specific opacity of matter. Using the continuity equation,
the ram pressure of the accreting plasma is now obtained as another function
of the radial distance (see Figure 4)
in contrast to the subcritical regime when 
.
Matching 
and 
(see the previous section) for the supercritical case gives (see inequality
(4.4.6))
The critical accretion rate 
is defined by the boundary of the inequality
and, correspondingly, is
The dependence of the Alfven radius on the accretion
rate is such that the Alfven radius (beyond the capture radius) slightly
decreases with increasing accretion rate as 
, while it decerases below the capture radius as 
and attains its lowest value (4.4.5)
for the critical accretion rate 
, beyond which it is independent of the external conditions.
We also note that in the supercritical regime, the pressure of the accreting
plasma increases more slowly (as 
) when approaching the magnetic rotator than the pressure of the relativistic
wind (as 
) ejected by it. This means that in the supercritical case a cavern
may exist even below the capture radius.
The estimates presented here, of course, are most suitable for the case
of disk accretion. In fact, the supercritical regime
seems to emerge most frequently under these conditions. This can be simply
understood. Indeed, the accretion rate is proportional to the square of
the capture radius 
. At the same time, the angular momentum of the captured matter is also
proportional to 
. Hence, at high accretion rates the formation of the disk looks natural.
