Sketches of possible scenarios that can inject CRs into NTFs. Left: a massive star located in the center drives a stellar wind that terminates at a shock. This shock accelerates CRs, which diffuse onto draped ISM magnetic fields, which experienced mixing with the shocked wind via Rayleigh–Taylor instabilities and escape into the ISM. Right: a pulsar drives the wind by accelerating electron–positron pairs toward the wind termination shock. Piled-up field lines behind the wind termination shock can reconnect with the ISM magnetic field, allowing CRs to escape.