tokens: and remain the same also in the saturated stage. The PDFs in the saturated stage are more intermittent than in the kinematic stage, but the PDFs both in the kinematic and saturated stages are more intermittent for the case than for any of the cases (compare the x -axis values and the heavy tails at higher values in Figs 5a and 8c ). However, the growth rate and the structure of the magnetic fields in the kinematic and saturated stages, even for the case, are unaffected by the configuration of the seed field. The overall conclusions, even with changes in the plasma parameters, remain the same as before: the structure and strength of the seed magnetic fields do not affect the growth rate, final saturation level, shape of the magnetic power spectrum, and the statistical structure of the small-scale dynamo generated magnetic fields. Thus, the detailed properties of the seed field or even their various generation mechanisms are relatively unimportant when studying evolved magnetic fields that were amplified by the turbulent small-scale dynamo. 4 DISCUSSION From our results, we show that the seed magnetic field information is lost (within a few eddy turnover times, as seen in Figs 2a , 6a , 7a , and 8a ). Then, the dynamo-generated magnetic field reaches a statistically similar state for all three seed fields, which is determined by the properties of the turbulence (such as Re and ) and magnetic resistivity (or equivalently Rm). This also shows that the small-scale dynamo is very efficient in amplifying (given that Rm is greater than its critical value, Rm (crit) ) any non-zero seed field. 4.1 Small-scale magnetic fields generated by the tangling of the large-scale field If Rm Rm (crit) , the small-scale dynamo is inactive. However, for the case with non-zero mean seed field (UniRm100), small-scale magnetic fields can still be generated by the tangling of the large-scale (or mean) uniform seed field (see appendix A in Seta et al. 2018 , for discussion on various mechanisms by which small-scale magnetic fields can be generated). Such a mechanism is only applicable in systems, such as spiral galaxies, where the large-scale field is maintained by other processes, i.e. α − Ω large-scale dynamo (Krause Rädler 1980 ; Shukurov Sokoloff 2008 ; Chamandy et al. 2014 ) or cosmic ray driven dynamo (Parker 1992 ; Hanasz et al. 2004 ). In our simulations, the large-scale uniform field is maintained at all times because the MHD equations (equations 1 – 4 ) preserve the net seed magnetic flux in a triply periodic numerical domain. We demonstrate the growth of small-scale magnetic fields by the tangling of the uniform seed field in Fig. 9 by choosing Rm = 100 Rm (crit) (≈165). In Fig. 9(a) , we show the evolution of magnetic and turbulent kinetic energies for models with all three seed field cases (UniRm100, PLRm100, and ParRm100). The magnetic energy only grows (linearly) for the case UniRm100 and decays for the other two cases (PLRm100 and ParRm100). Figure 9. Same
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