The Cosmic Symphony: Magnetic Fields and Turbulence Across Clouds, Galaxies, to Galaxy Clusters

Understanding turbulent magnetic fields in magnetized plasma is critical for modern astrophysical research. This understanding is essential for quantitatively describing key astrophysical processes, linking microscopic phenomena, such as cosmic ray transport and star formation, with the large-scale evolution of galaxies and clusters. This work comprehensively studies MHD turbulence anisotropy using analytical, numerical, and observational approaches. It resolves several long-standing puzzles, including the origin of observed neutral hydrogen striations, the escape of galactic cosmic rays perpendicular to the magnetic field, and the relative inefficiency of turbulent damping in partially ionized plasmas.

To measure 3D magnetic fields in the interstellar medium, this talk presents two innovative techniques based on turbulence anisotropy: the Velocity Gradient Technique and the physics-informed convolutional neural network. The talk will demonstrate how these techniques serve as transformative tools for probing 3D magnetic fields, advancing our understanding of the intricate interplay between turbulence and magnetism across cosmic scales. The new turbulence-based approach overcomes the limitations of traditional polarization measurements. It provides unprecedented insights into the magnetic field structure of various astrophysical systems, from accretion disks to the halos of galaxy clusters. It opens avenues for separating CMB polarization arising from enigmatic cosmological B-modes from the galactic foreground. Combined with numerical modeling, this research yields unique insights into the physics of matter accretion to supermassive black holes, star formation, and cosmic ray propagation.