Coordinated remote-sensing and in-situ observations of a flare source (lower left) producing a jet seen in UV and X-rays, which outline the loops and interactions at loop footpoints (blue). Escaping electrons produce a radio burst (upper right) whose frequency depends on the coronal height of the emitting particles. Subsequently, the energetic electrons are the first particles to arrive at the Solar Orbiter spacecraft, while the heavier energetic ions arrive later, and provide signatures of extreme fractionation produced by the acceleration mechanism. The prompt arrival of the particles establishes that Solar Orbiter is magnetically connected to the X-ray source, allowing comparison with coronal magnetic field models in the region of the active region (adapted from A. Benz, 3rd Solar Orbiter Workshop, Sorrento).