Volume 603, July 2017
|Number of page(s)||6|
|Section||Stellar structure and evolution|
|Published online||30 June 2017|
Energy distribution of relativistic electrons in the young supernova remnant G1.9+0.3
1 Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland
2 Max-Planck-Institut für Kernphysik, PO Box 103980, 69029 Heidelberg, Germany
3 MEPHI, Kashirskoe shosse 31, 115409 Moscow, Russia
Received: 7 December 2016
Accepted: 20 April 2017
The broad-band X-ray observations of the youngest known galactic supernova remnant (SNR), 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.
Key words: supernovae: individual: SNR G1.9+0.3 / gamma rays: ISM
© ESO, 2017
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