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

Abstract

Observations have shown that spatially extended "TeV halos" are a common (and potentially 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 interstellar medium, but smaller than expected in models of cosmic-ray diffusion through the standard interstellar medium. Several explanations have been proposed, but all have shortcomings. Here, we revisit a class of models where the cosmic-ray gradient produced by the central source induces a streaming stability that "self-confines" the cosmic-ray population. We find that previous studies significantly underpredicted the degree of cosmic-ray confinement and show that corrected models can significantly inhibit cosmic-ray diffusion throughout the TeV halo, especially when similar contributions from the coincident supernova remnant are included.

arXiv comment12 pages, 10 figures

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Cited by in corpus (30)

• The Physics of Pulsar Halos: Research Progress and Prospect
• Are pulsar halos rare ?
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• TeV halos and the role of pulsar wind nebulae as sources of cosmic ray positrons
• Ultra-High-Energy Gamma-Ray Astronomy
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• Self-confinement of relativistic pair beams in magnetized interstellar plasmas: the case of pulsar X-ray filaments
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• Investigating the emission signatures of pulsar halo candidate HESS J1813-126
• Stochastic modelling of cosmic-ray sources for Galactic diffuse emissions