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tokens: between the curves of Figure 6 (a) are due to this anisotropic and coherent velocity strength. The Fourier transform as a function of k y (not shown) is almost the same as Figure 6 (a). Figure 6 (c) shows the kinetic energy power spectrum as a function of ; the differences between the energy contribution of the modes in the cases with and without shear are more pronounced, but still rather small. We speculate that the action of the stress tensor (when the shear is applied) leads to an increase of mode contributions at all scales, but in particular near the diffusion region, increasing the reconnection rate; this is in agreement with Nakamura et al. ( 2008 ), who reported an enhancement of island production when shear was present. Figure 6. (a) Power spectra of the velocity as a function of k . (b) Velocity as a function of k x . (c) Kinetic energy as a function of k . For all cases the red line represents the fan stage at t = 303.0 s just before the shear is applied, and the blue one just after it, at t = 304.0 s. If we consider a magnetic configuration scheme (see Figure 1 of Paper I ), the setup described by Table 1 , and whose results are shown in Figure 4 , will represent the face-on view. To also consider the edge-on view, we perform another simulation where the initial magnetic field, instead of being homogeneous, is the CS given bywith B 0 = 3.0 G. The preparation of the fan is performed with the two stages as in the previous case, but in this case the shear (Equation ( 12 )) coincides with the CS location. The instantaneous pressure pulses are again applied at time t = 305.9 s. Figure 7 shows the temperature (i) and the density with overlapped magnetic field lines (ii) at an early time t = 312 s. The resulting pulse patterns are labeled ( E ), ( F ), ( G ), and ( H ). Figures 7 (c)–(d) show the same evolved patterns 1 minute later, at t = 372 s, for the temperature with magnetic field lines superimposed (iii) and the EM with temperature contours (iv). Same as before, the EM contrast of the SAD candidates will fade away fast and before the desired time if during their evolution they are not sufficiently isolated by the magnetic field. In fact, the feature ( F ) triggered in a location where the magnetic field lines are almost straight is not appreciated even at an early time (Figures 7 (a)–(b)). The cavities that survive and can be identified as SADs are located mainly in the neighborhood of the CS, 7 7 This is noted more clearly when the turbulence stage is carried out using larger wavenumbers compared with those chosen here. See also Paper I . where the magnetic field is rolled up, forming closed vortices and islands. Figure 7. (a) Temperature at t = 312 s; ( E ), ( F ), ( G ), and ( H ) labeled cavities triggered at t = 305.9 s. (b) Density at t = 312 s. Same as before, but with magnetic field lines superimposed. (c) Same as (i), but 1 minute later, at t = 372 s. (d) EM, also at t = 372 s. Cavities ( G ) and ( H ) have an EM