X-Ray Emission from the PeVatron-candidate Supernova Remnant G106.3+2.7
Abstract
We report a discovery of diffuse X-ray emission around the supernova remnant (SNR) G106.3+2.7, which is associated with VER J2227+608 and HAWC J2227+610 and is known as a candidate for a PeV cosmic ray accelerator (PeVatron). We analyze observational data of Suzaku around the SNR and the adjacent pulsar PSR J2229+6114. We find diffuse X-ray emission that is represented by either thermal or non-thermal one. However, the metal abundance for the thermal emission is <0.13 Z_sun, which may be too small in the Milky Way and suggests that the emission is non-thermal. The intensity of the diffuse emission increases toward PSR J2229+6114 in the same way as radio emission, and it is in contrast with gamma-ray emission concentrated on a molecular cloud. The X-ray photon index does not change with the distance from the pulsar and it indicates that radiative cooling is ineffective and particle diffusion is not extremely slow. The X-ray and radio emissions seem to be of leptonic origin and the parent electrons may originate from the pulsar or its wind nebula. The gamma-ray emission appears to be of hadronic origin because of its spacial distribution. The parent protons may be tightly confined in the cloud separately from the diffusing electrons.
Keywords
Cite
@article{arxiv.2101.10329,
title = {X-Ray Emission from the PeVatron-candidate Supernova Remnant G106.3+2.7},
author = {Yutaka Fujita and Aya Bamba and Kumiko K. Nobukawa and Hironori Matsumoto},
journal= {arXiv preprint arXiv:2101.10329},
year = {2021}
}
Comments
matched the published version