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We report four years of radio and X-ray monitoring of the Type IIn supernovaSN 2006jd at radio wavelengths with the Very Large Array, Giant Metrewave RadioTelescope and Expanded Very Large Array; at X-ray wavelengths with {\emChandra}, {\em XMM-Newton} and {\em Swift}-XRT. We assume that the radio andX-ray emitting particles are produced by shock interaction with a densecircumstellar medium. The radio emission shows an initial rise that can beattributed to free-free absorption by cool gas mixed into the nonthermalemitting region; external free-free absorption is disfavored because of theshape of the rising light curves and the low gas column density inferred alongthe line of sight to the emission region. The X-ray luminosity implies apreshock circumstellar density $\sim 10^6$ cm$^{-3}$ at a radius $r\sim 2\times10^{16}$ cm, but the column density inferred from the photoabsorption of X-raysalong the line of sight suggests a significantly lower density. The implicationmay be an asymmetry in the interaction. The X-ray spectrum shows Fe lineemission at 6.9 keV that is stronger than is expected for the conditions in theX-ray emitting gas. We suggest that cool gas mixed into the hot gas plays arole in the line emission. Our radio and X-ray data both suggest the densityprofile is flatter than $r^{-2}$ because of the slow evolution of theunabsorbed emission.

Radio and X-ray observations of SN 2006jd: Another strongly interacting Type IIn supernova