Supernova remnants (SNRs), generated from the evolution of a star, are considered promising sites for the generation of high energy particles and cosmic rays. The magnetic field in SNRs plays a key role in setting the energy of the emitted particles. Recently Moeri Tao and colleagues analysed the magnetic field of supernova SN 1006 (including both northeast and southwest shells) using the radiation emission in both radio and X-rays and found that the magnetic field strength is locally enhanced by a factor of approximately 100. This finding may explain the high-energy end of the emitted particle power spectrum.

Broadband radio data from the MeerKAT radio telescope (ranging from 1.37 GHz to 100 GHz) cannot be described by a single power law, since the spectral behaviour changes noticeably at a break frequency around 36 GHz. One plausible reason for such a feature is loss of synchrotron radiation due to cooling of electrons. This cooling break occurs when electron cooling time and dynamical timescale of the SNR are balanced. The break frequency corresponds to a magnetic field strength of more than 2 mG. The minimum magnetic field, of the order of 10 μG, is obtained from an equipartition between the electron and magnetic field energy densities.

恒星演化产生的超新星遗迹（SNR）被认为是产生高能粒子和宇宙射线的有希望的场所。信噪比中的磁场在设置发射粒子的能量方面起着关键作用。最近，Moeri Tao 及其同事利用无线电和 X 射线的辐射发射分析了超新星 SN 1006（包括东北壳层和西南壳层）的磁场，发现磁场强度局部增强了大约 100 倍。这一发现可以解释发射粒子功率谱的高能端。

来自 MeerKAT 射电望远镜（范围从 1.37 GHz 到 100 GHz）的宽带射电数据无法用单一幂律描述，因为频谱行为在 36 GHz 附近的拐点频率处发生显着变化。造成这种特征的一个可能的原因是由于电子冷却而导致同步加速器辐射的损失。当电子冷却时间和 SNR 的动态时间尺度达到平衡时，就会发生这种冷却中断。转折频率对应于超过 2 mG 的磁场强度。 10 μG 量级的最小磁场是通过电子和磁场能量密度之间的均分获得的。