On the energy distribution of relativistic electrons in the young supernova remnant G1.9+0.3

Abstract

The broad-band X-ray observations of the youngest known galactic supernova remnant, G1.9+0.3, provide unique information about the particle acceleration at the early stages of evolution of supernova remnants. Based on the publicly available X-ray data obtained with the Chandra and NuSTAR satellites over two decades in energy, we derived the energy distribution of relativistic electrons under the assumption that detected X-rays are of entirely synchrotron origin. The acceleration of electrons was found to be an order of magnitude slower than the maximum rate provided by the shock acceleration in the nominal Bohm diffusion regime. We discuss the implications of this result in the context of contribution of SNRs to the Galactic Cosmic Rays at PeV energies.

arXiv comment6 pages, 5 figures sibmitted to A&A

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Cited by in corpus (9)

• Radio Evolution of Supernova Remnants Including Non-linear Particle Acceleration: Insights from Hydrodynamic Simulations
• Systematic Study of Acceleration Efficiency in Young Supernova Remnants with Nonthermal X-ray Observations
• Non-thermal emission from the reverse shock of the youngest galactic Supernova remnant G1.9+0.3
• On the foundation of equipartition in supernova remnants
• NuSTAR observations of the supernova remnant RX J1713.7$-$3946
• Electron Acceleration in Middle-age Shell-type $\gamma$-Ray Supernova Remnants
• Leptonic or Hadronic Emission: X-Ray Radiation Mechanism of Large-scale Jet Knots in 3C 273
• Electron Energization in Quasi-Parallel Shocks: Test-Particle-Electrons in a Proton Driven Turbulence
• Brightening and Fading in the Youngest Galactic Supernova Remnant G1.9+0.3: 13 years of monitoring with the Chandra X-ray Observatory