  The appearance of subsonic propellers situated in a strong wind is discussed.
We show that it is similar to the appearance of anomalous X-ray pulsars (AXPs)
provided the mass and the magnetic moment of neutron stars are 1.4 solar
masses, and 2E+30 G cm^3, respectively, and the strength of the wind is M_c =
3E+17 g/s. Under these conditions, the spin periods of subsonic propellers are
limited within the range of 5-15 s, and the expected spin-down rates are close
to 7E-11 s/s. The mass accretion rate onto the stellar surface is limited to
the rate of plasma penetration into its magnetosphere at the boundary. As this
process is governed by the reconnection of the field lines, the accretion rate
onto the stellar surface constitutes 1-2% of M_c. In this case the X-ray
luminosity of the objects under consideration can be evaluated as 4E+35 erg/s.
The model predicts the existence of at least two spatially separated sources of
the X-ray emission: hot spots at the stellar surface, and the hot atmosphere
surrounding the magnetosphere of the star. The ages of the subsonic propellers
under the conditions of interest are limited to 10^5 yr.
