Diagnosing Turbulence in the Neutral and Molecular Interstellar Medium of Galaxies

Magnetohydrodynamic (MHD) turbulence is a crucial component of the current paradigms star formation, dynamo theory, particle transport, magnetic reconnection, and evolution structure in interstellar medium (ISM) galaxies. Despite importance to astrophysical fluids, full theoretical framework based on solutions Navier–Stokes equations remains intractable. Observations provide only limited line-of-sight information densities, temperatures, velocities, field strengths, therefore directly measuring ISM challenging. A statistical approach has been great utility allowing comparisons observations, simulations, analytic predictions. In this review article, we address growing MHD many fields astrophysics diagnostics for studying interplanetary turbulence. particular, will machine learning algorithms that have developed observational data sets order obtain about cascade, fluid compressibility (sonic Mach number), magnetization (Alfvénic number). These techniques often tested numerical simulations turbulence, which may include creation synthetic are formulated expectations compressible magnetized We stress use multiple techniques, as can more accurate indication parameters interest. conclude by describing several open-source tools community when dealing with