Abstract
G1.9+0.3 is the youngest known Galactic supernova remnant (SNR) and dominated by X-ray synchrotron emission. Synchrotron X-rays can be a useful tool to study the electron acceleration in young SNRs. The X-ray spectra of young SNRs give us information about the particle acceleration at the early stages of evolution of SNRs. In this work, we investigate the time evolution of roll-off frequency of the synchrotron spectrum from SNR G1.9+0.3 using Suzaku. For this analysis, we use ∼101 ks (2011) and ∼92 ks (2015) observations with the X-ray Imaging Spectrometer. We find that there is no significant differences in the spectral parameters and interpret our results.
Highlights
The X-ray spectra of several young supernova remnant (SNR) are dominated by non-thermal emission: e.g., SN 1006 [1], G347.3−0.5 [2, 3] and G266.2−1.2 [4]
The νFν spectrum of synchrotron X-ray emission has a peak around the roll-off frequency, νroll, which is related to the maximum electron energy of accelerated electrons (Emax,e) and the magnetic field (B), νroll ∝ Em2 ax,e B [10, 11]
In order to investigate the time variability of X-ray emission from G1.9+0.3, we extracted X-ray Imaging Spectrometer (XIS) spectra from a circular region at the source with a radius of 3.1 arcmin centered on the remnant for both data sets
Summary
The X-ray spectra of several young SNRs are dominated by non-thermal emission: e.g., SN 1006 [1], G347.3−0.5 [2, 3] and G266.2−1.2 [4]. 1. Introduction The X-ray spectra of several young SNRs are dominated by non-thermal emission: e.g., SN 1006 [1], G347.3−0.5 [2, 3] and G266.2−1.2 [4]. Their spectra have a power-law form (the synchrotron flux density at frequency ν is Fν ∝ ν−α ∝ ν1−Γx, where α is the spectral index and Γx is the photon index).
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