  Turbulent viscosity $\nu_t$ and resistivity $\eta_t$ are perhaps the simplest
models for turbulent transport of angular momentum and magnetic fields,
respectively. The associated turbulent magnetic Prandtl number $Pr_t\equiv
\nu_t/\eta_t$ has been well recognized to determine the final magnetic
configuration of accretion disks. Here, we present an approach to determining
these ''effective transport'' coefficients acting at different length-scales
using coarse-graining and recent results on decoupled kinetic and magnetic
energy cascades [Bian & Aluie 2019]. By analyzing the kinetic and magnetic
energy cascades from a suite of high-resolution simulations, we show that our
definitions of $\nu_t$, $\eta_t$, and $Pr_t$ have power-law scalings in the
''decoupled range.'' We observe that $Pr_t\approx1 \text{~to~}2$ at the
smallest inertial-inductive scales, increasing to $\approx 5$ at the largest
scales. However, based on physical considerations, our analysis suggests that
$Pr_t$ has to become scale-independent and of order unity in the decoupled
range at sufficiently high Reynolds numbers (or grid-resolution), and that the
power-law scaling exponents of velocity and magnetic spectra become equal. In
addition to implications to astrophysical systems, the scale-dependent
turbulent transport coefficients offer a guide for large eddy simulation
modeling.
