3D volume renderings of the magnetic field line distribution for the high-B (top panels) and low-B (bottom panels) cases are shown, with jet propagation angles Θ = 5° , 40° , 85° from left to right (Table 1). A common color scale (|B| in μG) is adopted to enable direct comparison of field strength and spatial distribution. Although the magnetic field remains dynamically subdominant within the explored parameter regime, it plays a critical role in shaping the emission properties. In particular, the high-B cases exhibit enhanced magnetic field concentration at the terminal shocks and a stronger presence within secondary structures, leading to observable differences in radio galaxy morphology. Regardless of magnetization level, the tangled field topology highlights the complexity of the cocoon environment, supporting the development of turbulence and providing favorable conditions for particle acceleration.