Results of the simple Kolmogorov-like case (see the parameters in Table 1). Top left: the current photon spectrum with the observational data (see Baldwin 1971; Baars et al. 1977; Macías-Pérez et al. 2010 for radio, Ney & Stein 1968; Grasdalen 1979; Green et al. 2004; Temim et al. 2006 for IR, Kuiper et al. (2001) for X-rays, and Aharonian et al. 2006; Albert et al. 2008; Abdo et al. 2010 for γ-rays). Top right: evolution of the particle spectra from ﹩{10}^{-2}{t}_{\mathrm{age}}=9.5\,\mathrm{years}﹩ (dotted red) to t_age = 950 years (thick green) with the result of TT10 at t_age (thin black). Bottom left: timescales of the acceleration ﹩{t}_{\mathrm{acc}}(\gamma ,t)={\gamma }^{2}/2{D}_{\gamma \gamma }(\gamma ,t)﹩ (positive slope red line), synchrotron cooling ﹩{t}_{\mathrm{syn}}=\gamma /{\dot{\gamma }}_{\mathrm{syn}}﹩ (negative slope blue lines), and the inverse Compton cooling ﹩{t}_{\mathrm{IC}}=\gamma /{\dot{\gamma }}_{\mathrm{IC}}﹩ (concave upward green line) for different ages. Only t_syn changes with time in this case (the thin, dotted, and thick lines correspond to ﹩{10}^{-2}{t}_{\mathrm{age}}﹩, ﹩{10}^{-1}{t}_{\mathrm{age}}﹩, and t_age, respectively). Bottom right: evolution of the fractional energy of the particles ﹩\int d\gamma \gamma {m}_{{\rm{e}}}{c}^{2}N(\gamma ,t)﹩ (thick blue), magnetic field η_BE_rot(t) (dot–dot dashed yellow,  amplified times 10), of the radiated and wasted ones by synchrotron (dotted red), inverse Compton (dotted–dashed purple, 10² times amplified), and adiabatic (dashed green) cooling ﹩{\int }_{0}^{t}{dt}^{\prime} \int d\gamma | {\dot{\gamma }}_{i}(\gamma ,t^{\prime} )| {m}_{{\rm{e}}}{c}^{2}N(\gamma ,t^{\prime} )﹩ (i = syn, IC, ad) and of the sum of all of them (thin black). All the components are divided by E_rot(t), which is increasing with time.