AI 中文总结
该研究通过一维PIC模拟揭示共振逆康普顿散射驱动的对级联在磁星磁层中形成单半球加速间隙，导致不对称硬X射线产生，为相位分辨光谱提供预测。
AI 中文摘要
持续磁星发射中的硬X射线来源于对负载磁层等离子体中的辐射过程，然而对这种辐射丰富系统的自洽动理学模拟仍然有限。我们进行了沿扭曲磁层中孤立场线、由共振逆康普顿散射（RICS）介导的对产生的一维粒子网格（PIC）模拟，从第一性原理出发捕捉粒子加速和辐射阻力。阻力强烈依赖于粒子洛伦兹因子和位置，在磁层电路中起关键作用。强的RICS阻力阻碍电子和正电子的流动，尤其是在延伸场线上。尽管如此，等离子体通过在一个半球中靠近恒星处自组织成一个单一的加速间隙来维持电路。来自间隙的加速等离子体流在延伸的RICS区域中负载大量电子-正电子对，同时还携带从恒星提取并在间隙中加速的离子。当辐射阻力在磁赤道处阻止对负载流时，离子成分通过流不稳定性传递动量，将少量轻子群体输送到相反半球并维持电路。局限于单个（阳极）半球的间隙意味着不对称的硬X射线产生，可能在相位分辨磁星光谱中探测到。
英文摘要
Hard X-rays in persistent magnetar emission originate from radiative processes in pair-loaded magnetospheric plasma, yet self-consistent kinetic simulations of such radiation-rich systems remain limited. We perform 1D particle-in-cell simulations of pair creation mediated by resonant inverse Compton scattering (RICS) along isolated field lines in twisted magnetospheres, capturing particle acceleration and radiative drag from first principles. The drag force, which strongly depends on the particle Lorentz factor and location, plays a key role in the magnetospheric circuit. Strong RICS drag impedes the flow of electrons and positrons, particularly along extended field lines. Nevertheless, the plasma sustains the circuit by self-organizing into a single accelerating gap near the star in one hemisphere. The accelerated plasma flow from the gap becomes loaded with copious electron-positron pairs in extended RICS zones, and also carries ions extracted from the star and accelerated in the gap. When radiative drag stops the pair-loaded flow at the magnetic equator, the ion component transfers momentum through streaming instabilities, delivering a small lepton population into the opposite hemisphere and sustaining the circuit. The gap confined to a single (anode) hemisphere implies asymmetric hard X-ray production, possibly detectable in phase-resolved magnetar spectra.
Comments15 pages, 8 figures, submitted to ApJL
