Simulating Rayleigh-Taylor induced magnetohydrodynamic turbulence in prominences

Solar prominences represent large-scale condensations suspended against gravity within the solar atmosphere. The Rayleigh-Taylor (RT) instability is proposed to be one of important fundamental processes leading generation dynamics at many spatial and temporal scales these long-lived, cool, dense structures amongst corona. We run 2.5D ideal magnetohydrodynamic (MHD) simulations with open-source MPI-AMRVAC code far into nonlinear evolution an RT perturbed prominence-corona interface. Our simulation achieves a resolution down $\sim 23$ km on 2D $(x,y)$ domain size 30 Mm $\times$ Mm. follow transitioning from multi-mode linear perturbation its nonlinear, fully turbulent state. Over succeeding 25$ minute period, we perform statistical analysis prominence cadence 0.858$ s. find dominant guiding $B_z$ component induces coherent structure formation predominantly in vertical velocity $V_y$ component, consistent observations, demonstrating anisotropic turbulence state our prominence. power-law scalings inertial range for velocity, magnetic, temperature fields. presence intermittency evident probability density functions field fluctuations, which depart Gaussianity as consider smaller scales. In exact agreement, higher-order quantify multifractality, addition different scale characteristics behavior between longitudinal transverse directions. Thus, statistics remain conclusions previous observational studies, enabling us directly relate found quiescent