We study the launching of magnetized jets from a resistive circumstellar disk within a binary system, employing a unique combination of 3D MHD jet launching simulations (PLUTO code) and post- processed 3D radiative transfer modeling (RADMC-3D code). Our findings reveal a well-defined jet originating from the inner region of the disk, extending to a larger disk area. While the model attains steady states for a single star, a binary system leads to the emergence of tidal effects such as the formation of “spiral arms” in the disk and inside the jet. Here we have consistently implemented a time-dependent Roche potential for the gravity of the binary. As a major step forward, we further present the first 3D radiation maps of the dust continuum for the disk-jet structure. In principle, this allows us to compare MHD simulation results to observed disk-outflow features. We, therefore, present convolved images of the dust continuum emission, employing exemplary point spread functions of the MIRI instrument (5 μm band) and the ALMA array (320 μm band). In these bands, we identify distinguishable features of the disk-jet structure, such as ”spiral arms,” which we have also seen in the MHD dynamics. For gas density increased by an order of magnitude, the disk become optically thick at 5 μm, but remains bright at 320 μm. At this wavelength, 320 μm, enhanced structural features in the disk and the base of the wind become more pronounced and are well resolved in the convolved image.

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