even more. Such a strong magnetic field leads to both deceleration of the rotation of the fast-rotating compact object on a time scale of seconds and generation of a strongly magnetized wind that flows away from the object at a relativistic speed, $\Gamma_0\simeq 10^2-10^3$ (e.g., [@Usov94a]). The outflowing wind is Poynting flux–dominated, i.e., $\sigma = L_{\pm}/
L_{_P}\ll 1$, where

$$L_{_P}\simeq {2\over 3} {B_{_S}^2R^6\Omega^4\over c^3}\simeq 2\times
10^{52}\left({B_{_S}\over  10^{16}\,\,{\rm G}}
\right)^2\left({R\over 10^6\,\,{\rm cm}}\right)^6
\left({\Omega\over 10^4\,\,{\rm s}^{-1}}\right)^4\,\,
{\rm ergs\,\,s}^{-1}$$

is the luminosity of the compact object in the Poynting flux, $ L_{\pm}$ is its luminosity in both electron-positron pairs and radiation, $c$ is the speed of light, $R$ is the radius of the compact object and $\Omega$ is its angular velocity; $R\sim 10^6$ cm and $\Omega\sim 
10^4$ s$^{-1}$ for both millisecond pulsars and post-merger objects. For compact objects with extremely strong magnetic fields, $B_{_S}\sim 10^{16}$ G, it is expected that $\sigma $ is $\sim 0.01-0.1$ ([@Usov94a]).

A plausible magnetic topology for a relativistic magnetized wind outflowing from an oblique rotator ($\vartheta\neq 0$) with a nearly dipole magnetic field is shown in Figure 1, where $\vartheta$ is the angle between the rotational axis and the magnetic axis. Near the rotational poles, the wind field 