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In order to gain a better understanding of the influence of cosmic rays (CRs)and magnetic fields in the disk-halo interface of edge-on spiral galaxies, weinvestigate the radio continuum halo, the magnetic field, and the transportprocesses of the CRs of the edge-on spiral galaxy NGC 4217 using CHANG-ES radiodata at two frequencies, 6 GHz (C-band) and 1.5 GHz (L-band), and supplementalLOFAR data at 150 MHz and X-ray Chandra data.  NGC 4217 shows a large-scale X-shaped magnetic field structure, covering amajor part of the galaxy with a mean total magnetic field strength in the diskof 9 micro Gauss (via equipartition). Using rotation measure synthesis(RM-synthesis) at C-band, we found that the direction of the disk magneticfield is pointing inward. A helical outflow structure is furthermore present inthe northwestern part of the galaxy, which is extended nearly 7 kpc into thehalo. More polarized emission is observed on the approaching side of thegalaxy. With a simplified galaxy disk model, we are able to explain thatfinding and predict that roughly 75% of edge-on spiral galaxies will showhigher polarized intensity on the approaching side. Many loop and shellstructures are found throughout the galaxy in total intensity at C-band. Asuperbubble-like structure is prominent in total and polarized intensity, aswell as in Halpha and optical dust filaments, being a possible result ofconcentrated star formation in the disk. The flux density contribution of thedisk in comparison to the halo decreases toward lower frequencies. Totalintensity profiles at the three radio frequencies were fit with two-componentexponential functions. The frequency dependence of the resulting scale heightsbetween C-band and L-band suggests advection to be the main CR transportprocess. The 1D CR transport modeling (SPINNAKER) shows that advection appearsto be more important than diffusion.

CHANG-ES XXI. Transport processes and the X-shaped magnetic field of NGC 4217: off-center superbubble structure