to the mean energy of protons, i.e. up to $\sim m_pc^2 \Gamma_0$ (see Fig. 3). At $\alpha_{\rm cr} < \alpha \lesssim 1$, the mean Lorentz factor of outflowing high-energy electrons after their reflection and acceleration at the barrier front depends on $\alpha$ and is

$$\langle\Gamma_e^{\rm {out}}\rangle \simeq 0.2
\left(\frac{m_p}{m_e}\right)\Gamma_0
\label{Gammamean}$$

within a factor of 2. The total energy of accelerated electrons is about 20% of the energy in outflowing protons which are reflected from the magnetic barrier.

5\. At $\alpha_{\rm cr} < \alpha \lesssim 1$, the mean Lorentz factor of protons reflected from the barrier is $\langle \Gamma_p^{\rm{out}}\rangle \simeq (0.7\pm 0.1)\Gamma_0$, i.e. the process of the beam proton reflection from the barrier is non-elastic, and about 30% of the initial kinetic energy of the beam protons is lost in this collision. The energy that is lost by the beam protons is transferred to high-energy electrons and low-frequency electromagnetic waves. Typically, the energy in these waves is a few times smaller than the energy in high-energy electrons.

In the burster frame, a magnetized wind flows away from the burster at relativistic speeds and collides with an ambient medium. In the process of such a collision, the outflowing wind loses its energy. 