Modeled source region of the solar wind and comparison to observations. (a) Vertical component of magnetic field in the photosphere of the 3D MHD model. (b) Coronal emission synthesized from the model in the 174 Å passband integrated along the vertical direction, corresponding to an observation near the center of the solar disk. (c) Same as (b) but integrated along the horizontal (Y) direction, corresponding to an off-limb observations. (d) Coronal observation of the source region of the wind at the limb with HRI_EUV on board Solar Orbiter at 174 Å (at 04:49:21 UT on 2022 March 30). The white arrows mark the location of (inverse-Y-type) jets, one example in the observation, and a comparable jet in the model. The field of view of model and observation in (c) and (d) is the same. The intensity maps are shown on a logarithm scale with arbitrary units. An animation is available online.