The curved spectrum of the young pulsar halo LHAASO J0248+6021 is explained by a time-dependent energy-loss bump in the electron spectrum that remains close to the cutoff, unifying it with the shifted bump observed in the older Geminga halo.
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Anisotropic diffusion modeling of HAWC pulsar halo morphologies constrains mean magnetic field orientations, Alfvénic Mach numbers near 0.2, and a local coherence length of ~100 pc for Geminga and Monogem.
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Spectral energy-loss bump and $\gamma$-ray pulsar halos
The curved spectrum of the young pulsar halo LHAASO J0248+6021 is explained by a time-dependent energy-loss bump in the electron spectrum that remains close to the cutoff, unifying it with the shifted bump observed in the older Geminga halo.
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Anisotropic Diffusion in Pulsar Halos: Interpreting the asymmetric morphology of Geminga and Monogem halos measured by HAWC
Anisotropic diffusion modeling of HAWC pulsar halo morphologies constrains mean magnetic field orientations, Alfvénic Mach numbers near 0.2, and a local coherence length of ~100 pc for Geminga and Monogem.