Preface

Dark Matter Particle Explorer observations of high-energy cosmic ray electrons plus positrons and their physical implications

“…Astrophysically it is not easy to generate quasi-monochromatic spectra. We found a possible exception is the cold, ultra-relativistic e + e − plasma wind from pulsars [129][130][131]. The Lorentz factor of the bulk flow of pulsar winds is suggested to be ∼ 10 6 , which just corresponds to the energy of the DAMPE peak.…”

Comptonization of Cosmic Microwave Background by Cold Ultrarelativistic Electron-Positron Pulsar Wind and Origin of ~130 GeV Lines

“…The model of [1] is based on inverse Compton scattering of energetic (UV and X-ray) photons by a cold ultrarelativistic e + -e − pulsar wind accelerated in the vicinity of pulsar magnetosphere, see e.g. [13] for details.…”

“…Previous claims about the presence of narrow line-like γ-ray feature(s) around 100-130 GeV observed by Large Area Telescope (LAT) on-board Fermi gamma-ray observatory near the Galactic Centre have been received a lot of attention. Proposed interpretations include dark matter annihilation [5][6][7][8][9], dark matter decay [9][10][11], systematic effects [2][3][4] and an astrophysical mechanism -comptonization (in deep Klein-Nishina regime) of cold ultra-relativistic e + -e − pulsar wind by external UV/X-ray emission [1].…”

“…In this paper, we discuss the astrophysical mechanism proposed by [1] in more details. We show that, in addition to ∼100 GeV line emission, it should produce broad γ-ray component due to comptonization of cosmic microwave background (CMB) radiation.…”

“…

Previously, [1] proposed an astrophysical explanation of narrow gamma-ray line-like feature(s) at ∼ 100 GeV from Galactic Center region observed by Fermi/LAT [2]. The model of [1] is based on the inverse Compton scattering of external ultra-violet/X-ray radiation by a cold ultra-relativistic e + -e − pulsar wind.

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