wind is about

$$B\simeq B_{_S}\frac {R^3}{r_{\rm lc}^2r}
\simeq  10^{15}\frac Rr\left(
\frac{B_{_S}}{ 10^{16}\,\rm{G}}\right) \left(\frac\Omega
{10^4\,\rm{s}^{-1}}\right)^2\rm{G},
\label{Bobj}$$

where $r_{\rm lc}=c/\Omega=3\times 10^6(\Omega /10^4\,$s$^{-1})$ cm is the radius of the light cylinder.

Non-thermal radiation from a relativistic strongly magnetized wind depends on whether the wind is striped in the direction of its outflow or not. If the wind is striped (see Fig.1), the magnetic field is more or less frozen in the outflowing plasma at the distance $r\lesssim r_f$ ([@Usov94a]; [@Blackman98]), where

$$r_f\simeq 2\times 10^{14} \sigma^{3/4}\left(
{B_{_ S}\over  10^{16}\,{\rm G}}\right)^{1/2}
\left({\Omega\over 10^4\,{\rm s}^{-1}}\right)^{1/2}\,\,
{\rm cm}\,.
\label{rnth}$$

At $r > r_f$, the wind density is not sufficient to screen displacement currents, and the striped component of the wind field is transformed into large-amplitude electromagnetic waves (LAEMWs) due to development of magneto-parametric instability ([@Usov75b], 1994a,b; Blackman et al. 1996; [@Melatos96]). \[For a criterion for electromagnetic waves to be considered as LAEMWs see § 4.\] The typical frequency of generated LAEMWs is equal to $\Omega$, and their amplitude is $\sim B$. Outflowing particles are accelerated in the field of LAEMWs to Lorentz factors of the order of $10^6$, and generate non-thermal synchro–Compton radiation with the typical energy of photons in the range of a few $\times (0.1-1)$ 