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 M \simeq 1.4 M _ { \sun } , and \mu \simeq 2 \times 10 ^ { 30 } { G cm ^ { 3 } } , respectively , and the strength of the wind is \dot { M } _ { c } \simeq 3 \times 10 ^ { 17 } { g s ^ { -1 } } .
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 \dot { P } \simeq 7 \times 10 ^ { -11 } { s s ^ { -1 } } .
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 \dot { M } _ { c } .
In this case the X-ray luminosity of the objects under consideration can be evaluated as L _ { X } \sim 4 \times 10 ^ { 35 } { erg s ^ { -1 } } .
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 \la 10 ^ { 5 } yr .