AI 中文总结
本研究通过对FRB 20220529的3.2年监测，发现其暴能量分布的特征标度E₀在暴率大幅下降时保持不变，为超高磁化中子星环境的相对论性重联提供了观测基准。
AI 中文摘要
快速射电暴（FRBs）是明亮的毫秒级射电瞬变现象，其物理起源仍未明确。一项关键诊断是，它们的暴能量分布是否保留了单个辐射源内部固有的、时间稳定的特征物理标度。在此，我们报告利用FAST和Parkes望远镜对高活跃重复FRB 20220529开展的3.2年监测活动，获得了1300余起暴，其谱能量密度跨度近5个数量级。累积暴率分布由指数加幂律（EXP+PL）形式描述，将具有特征标度（E₀）的低能指数分量与无标度的亮端尾端关联起来。尽管暴率下降超过一个数量级，该标度仍保持不变，揭示出与源的宏观触发活动解耦的稳定耗散标度。在磁星解释框架下，这一现象与扭曲磁球中局域亚临界重联事件与等离子体团介导的磁雪崩共存的情况一致。不变量E₀将耗散区域限制在内部至中层磁球，揭示了重复FRBs可变活动之下的稳健能量释放层级，为超高磁化中子星环境中的相对论性重联提供了观测基准。
英文摘要
Fast radio bursts (FRBs) are luminous millisecond radio transients whose physical origin remains unsettled. A key diagnostic is whether their burst-energy distributions retain characteristic physical scales that are intrinsic and temporally stable within an individual engine. Here we report a 3.2-year monitoring campaign of the hyperactive repeater FRB~20220529 with FAST and Parkes, yielding more than 1,300 bursts spanning nearly five orders of magnitude in spectral energy density. The cumulative burst-rate distribution is described by an exponential-plus-power-law (EXP+PL) form, linking a low-energy exponential component with characteristic scale (E_0) to a scale-free bright-end tail. This scale remains invariant despite the burst rate declining by more than an order of magnitude, revealing a stable dissipation scale decoupled from the source's macroscopic trigger activity. Within a magnetar interpretation, this phenomenology is consistent with localized sub-critical reconnection episodes coexisting with plasmoid-mediated magnetic avalanches in a twisted magnetosphere. The invariant (E_0) constrains the dissipation region to the inner-to-middle magnetosphere and reveals a robust energy-release hierarchy beneath the variable activity of repeating FRBs, providing an observational benchmark for relativistic reconnection in an ultra-magnetized neutron-star environment.
Comments38 pages, 9 figures
