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Observations have shown that spatially extended "TeV halos" are a common (andpotentially generic) feature surrounding young and middle-aged pulsars.However, their morphology is not understood. They are larger than the "compact"region where the stellar remnant dominates the properties of the interstellarmedium, but smaller than expected in models of cosmic-ray diffusion through thestandard interstellar medium. Several explanations have been proposed, but allhave shortcomings. Here, we revisit a class of models where the cosmic-raygradient produced by the central source induces a streaming stability that"self-confines" the cosmic-ray population. We find that previous studiessignificantly underpredicted the degree of cosmic-ray confinement and show thatcorrected models can significantly inhibit cosmic-ray diffusion throughout theTeV halo, especially when similar contributions from the coincident supernovaremnant are included.

Self-Generated Cosmic-Ray Turbulence Can Explain the Morphology of TeV Halos