Spectral energy distribution (energy flux versus energy, SED) of the γ-rays from the IC process and X-rays from the synchrotron process, produced by electrons accelerated in the wind collision region in the binary systems: PSR J1816+4510 (right column), PSR J1810+1744 (right-middle column), PSR J1023+0038 (left-middle column), and PSR B1957-20 (left column). a) Dependence on different advection velocities of the mixed pulsar-stellar winds: v_adv = 10¹⁰ cm s^-1 (dashed), 3 × 10⁹ cm s^-1 (solid), and 10⁹ cm s^-1 (dotted). The other parameters are fixed on σ = 10^-3, − 0.5 ≤ cosβ ≤  − 0.4. The differential spectrum of electrons is assumed to be a power-law type (spectral index − 2) between the maximum energy given by Eq. (7) and minimum energy equal to E_min = 0.5 GeV. The power in this electron spectrum is normalized to 1% of the pulsar rotational energy lost by the pulsar. b) Dependence on magnetization parameter of the pulsar wind: σ = 10^-2 (dotted), 10^-3 (solid), and 10^-4 (dashed). The other parameters are fixed on − 0.5 ≤ cosβ ≤  − 0.4 and E_e given by Eq. (7), and v_adv = 3 × 10⁹ cm s^-1. c) Dependence on the cosine of the observation angle (measured from the direction defined by the centers of the stars): 0.9 ≤ cosβ ≤ 1.0 (dashed, outwards from the companion star), 0.5 ≤ cosβ ≤ 0.6 (solid), − 0.1 ≤ cosβ ≤ 0 (dotted), − 0.5 ≤ cosβ ≤  − 0.4 (dot-dashed), − 1.0 ≤ cosβ ≤  − 0.9 (dot-dot-dashed), the electron energy E_e is given by Eq. (7), σ = 10^-3, and v_adv = 3 × 10⁹ cm s^-1.