Comparison of the median Brunt-Väisälä frequency ω_BV radial profiles and the median magnetic anisotropy profiles for all TNG-Cluster halos at z = 0. The solid lines and left y-axis depict ω_BV, while the dashed lines and right y-axis show the magnetic anisotropy β_A. Each median line and 16th to 84th percentile band is colored according to CC status. The horizontal dotted gray lines indicate exemplary constant stirring frequencies ω_stir in the same units as ω_BV, i.e., 1/Gyr. Gravity waves can be exited in regions with ω_stir < ω_BV and are reflected or trapped at a radius where ω_stir = ω_BV. The maximum of ω_BV, beyond the core, where gravity waves can be most easily trapped, and the minimum in β_A, where magnetic fields show the strongest tangential orientation, appear at similar radii, suggesting that gravity wave trapping can be effective for SCC clusters.