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.

12 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 ?
• Anisotropic diffusion cannot explain TeV halo observations
• Population synthesis of pulsar wind nebulae and pulsar halos in the Milky Way -- Predicted contributions to the very-high-energy sky
• TeV halos and the role of pulsar wind nebulae as sources of cosmic ray positrons
• Ultra-High-Energy Gamma-Ray Astronomy
• Geminga's pulsar halo: an X-ray view
• Galactic Diffuse Neutrino Emission from Sources beyond the Discovery Horizon
• Gamma-ray halos around pulsars: impact on pulsar wind physics and galactic cosmic ray transport
• Prospect of detecting TeV halos with LHAASO: in the framework of the anisotropic diffusion model
• The self-confinement of electrons and positrons from dark matter
• Features of the gamma-ray pulsar halo HESS J1831$-$098
• Effect of magnetic field correlation length on the gamma-ray pulsar halo morphology under anisotropic diffusion
• Constraining the slow-diffusion zone size and electron injection spectral index for the Geminga pulsar halo
• Disclosing the catalog pulsars dominating the Galactic positron flux
• Extended TeV Halos May Commonly Exist around Middle-Aged Pulsars
• Absence of TeV halos around millisecond pulsars
• Anisotropic Diffusion of $e^{\pm }$ in Pulsar Halos over Multiple Coherence of Magnetic Fields
• Regions of suppressed diffusion around supernova remnants?
• Detecting and characterizing pulsar haloes with the Cherenkov Telescope Array
• The environment of TeV halo progenitors
• PHECT: A lightweight computation tool for pulsar halo emission
• The traveling-PWN modeling attempt on the enigmatic LHAASO dumbbell-like structure
• Diagnosing Interstellar Magnetic Turbulence with TeV Pulsar Halos
• New estimate for the contribution of the Geminga pulsar to the positron excess
• Mirage Sources and Large TeV Halo-Pulsar Offsets: Exploring the Parameter Space
• Self-confinement of relativistic pair beams in magnetized interstellar plasmas: the case of pulsar X-ray filaments
• Method for testing diffusive shock acceleration and diffusion propagation of 1-100 TeV cosmic electrons with multiwavelength observations of the Geminga halo and pulsar wind nebula
• Investigating the emission signatures of pulsar halo candidate HESS J1813-126
• Stochastic modelling of cosmic-ray sources for Galactic diffuse emissions