[@OsborneEtAl1988; @SeoEtAl1994; @JonesEtAl2001], which is implemented in  such that $K_{pp}(R,\vec{x})=2\,h\,\delta(z)\,K_{pp}(R)$, and \[eq:Kpp\] K(R)K\_[pp]{}(R) = V\_[A]{}\^2 , where $V_{\rm A}$ is an effective Alfvénic speed characterizing the magnetic turbulence—$\delta$ is the diffusion spectral index in the intermediate inertial regime. Since it appears explicitly only as a normalization factor, we stick to this formula even when spatial diffusion exhibits several spectral regimes. The fact that reacceleration is [*effectively*]{} localized in the disk allows us to partly solve analytically, which significantly speeds up the numerical exploration of the parameter space [@Maurin2018]. While this “pinching” is a fair approximation for ionization and Coulomb processes, it is only a convenient approximation for adiabatic losses induced by convection and reacceleration. Hence, care should be taken when comparing inferred values of the parameters $V_{\rm c} \equiv | \vec{V}_{\rm c}|$ and $V_{\rm A}$ with theoretical expectations. Loosely speaking, one can expect to recover the phenomenology of a more extended reacceleration zone by a rescaling of $V_{\rm A}^2$ by a factor $h/z_{\rm A}$ [@MaurinEtAl2002], where $z_{\rm A}$ is the half-height over which reacceleration would spread in the magnetic slab [@JonesEtAl2001]. So, for $h/z_{\rm A}\simeq {\cal O}(h/L)$, our fitted value of $V_{\rm A}$ should be scaled by a factor $\sqrt{L/h}$ 