690c690
<     \eta_\mathrm{ACC} \equiv \frac{\sigma^3}{\mu_{50}^3 k_0^3} \eta_\lambda^{-2} \simeq \frac{2\sigma^3}{{\bar \rho} \lambda \mu_{50}^2 . } \label{etaacck0>mu50}
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>     \eta_\mathrm{ACC} \equiv \frac{\sigma^3}{\mu_{50}^3 k_0^3} \eta_\lambda^{-2} \simeq \frac{2\sigma^3}{{\bar \rho} \lambda \mu_{50}^2 } =\KK{ \frac{2 \sigma^3 v_\lambda^2}{\mu_{50}^4}.}  \label{etaacck0>mu50}
1567,1568c1567,1569
< \Fig{pkmax_comp_1024a_mu05_k002o} for an example where $\mu_{50}=0.5$
< and $k_0=1$.
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> \Fig{pkmax_comp_1024a_mu05_k002o} for \KK{Run S}, as an example, 
> % where $\mu_{50}=0.5$ and $k_0=1$.
> \KK{where we see the crossing of $\mu_5$ and $k_{\rm I}$.} 
1571c1572,1574
< We therefore speculate that the magnetic helicity-conserving phase is
---
> \KK{These observations would also suggest}
> %We therefore speculate 
> that the magnetic helicity-conserving phase is
1573c1576
< the adapted Hosking integral discussed in the beginning of the paper.
---
> the adapted Hosking integral \KK{as discussed in Sec.~\ref{IIE}}. %the beginning of the paper.
1585c1588,1592
< Namely, we }
---
> Namely, the system is frozen until $\eta=\eta_\lambda$ 
> and then evolve with the usual inverse cascade for the helical magnetic field
> as an intermediate stage until $\eta=\eta_\mathrm{ACC}$. 
> Then start to evolve with the decay law determined by the conservation
> of the adapted Hosking integral.}