time before hitting the disk within a radial distance $R < 10 R_{\star}$ (here we chose $R_{\star} = R_\odot = 6.957 \times 10^5 ~{\rm km} = 4.6 \times 10^{-3} $ AU).

Solar wind [*in-situ*]{} measurements at a variety of helio-latitudes by [*Helios, IMP 8*]{} and [*Ulysses*]{} [@Horbury.etal:96 see Fig. 4 therein] have shown a decrease of the correlation length of the turbulence, $L_c$, i.e., the scale of the injection of the turbulence (see Fig. \[Pspectrum\]), between a distance from the Sun of $\sim 1$ AU ($L_c \simeq 0.01$ AU) sun-ward down to $\sim 0.1$ AU ($L_c < 0.001$ AU). In the absence of current observational estimates of $L_c$ within a T Tauri wind close to the star, at distances $R < 10 R_{\star} < 0.1$ AU the range $L_c = 10^{-6}$–$10^{-4}$ AU (or $2.2 \times 10^{-4}$–$2.2 \times 10^{-2} R_\star$) seems to be a reasonable approximation. Based on solar wind observations, that represent one single realization of the unperturbed field and of the turbulence, it is hard to identify a correlation between $L_c$ and the field magnitude $B_0$. It is then not obvious that the strong field of a T Tauri star would lead to a different $L_c$. On the other 