Speaker
Description
Supernova remnants (SNRs) are widely regarded as the primary sources of Galactic cosmic rays, with particles accelerated at their shock fronts through the diffusive shock acceleration (DSA) mechanism, gaining energy via repeated shock crossings. Magnetic turbulence plays a crucial role in scattering these particles, making its characterization essential for understanding the acceleration process. In this study, we apply the two-point correlation method to derive the magnetic energy spectrum from the non-thermal X-ray flux image of Tycho’s SNR. The non-thermal flux image is obtained using Poissonian-based Generalized Morphological Component Analysis (pGMCA). The turbulence length scale inferred from the resulting magnetic energy spectrum is smaller than that derived from previous radio studies of Tycho’s SNR. Additionally, we estimate the magnetic energy spectrum using the X-ray rim thickness measured across the remnant, which serves as a proxy for the magnetic field strength. The turbulence scale derived from this approach is consistent with the magnetic energy spectrum obtained from the non-thermal X-ray flux analysis.
| Participate the oral/poster presentation award competition | Yes |
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