Diagnosing the particle transport mechanism in the pulsar halo via X-ray observations

• DOI: 10.48550/arxiv.2401.17982
• Publication Date: 2024-01-31
• Authors: Qi-Zuo Wu; Chao-Ming Li; Xuan-Han Liang; Chong Ge; R. Liu
• Keywords: Particle (ecology)

Pulsar halos (also termed 'TeV halo') are a new class of $\gamma$-ray sources in Galaxy, which manifest as extended emission around middle-age pulsars, discovered the Geminga pulsar, Monogem pulsar and PSR~J0622+3749 by HAWC LHAASO. A consensus has been reached that TeV comes from inverse Compton scattering escaping electrons/positrons PWN off soft background radiation field, while particle transport mechanism halo is still dispute. Currently, there mainly three interpretations, namely, isotropic, suppressed diffusion model; unsuppressed model with considering ballistic propagation newly injected particles; anisotropic model. While predicted gamma-ray surface brightness profiles all models can be more or less consistent observation, implication for cosmic-ray mechanisms properties interstellar magnetic field quite different. In this study, we calculate anticipated X-ray under models. We show synchrotron these electrons produce corresponding expected distinct suggest sensitive detectors large view (such eROSITA Einstein Probe) reasonably long exposure time crucial to understand formation serve probe turbulence.