Charged particles scattering on moving inhomogenities of the magnetised interstellar medium as can gain energy through the process of second-order Fermi acceleration. This energy gain depletes in turn the magnetic wave spectrum around the resonance wave-vector $k\sim 1/R_L$, where $R_L$ is the Larmor radius of the charged particle. This energy transfer can prohibit the cascading of magnetic turbulence to smaller scales, leading to a drop in the diffusion coefficient and allowing the efficient exchange of charged dark matter particles in the disk and the halo. As a result, terrestial limits from direct detection experiments apply to charged dark matter. Together with the no-observation of a drop in the diffusion coefficient, this excludes charged dark matter for $10^2 GeV\lesssim m/q \lesssim 10^{11} GeV$, even if the charged dark matter abundance is only a small part of the total relic abundance.

中文翻译：

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带电暗物质的再加速

带电粒子散射在磁化星际介质的移动不均匀性上，可以通过二阶费米加速过程获得能量。这种能量增益反过来消耗了共振波矢量 $k\sim 1/R_L$ 周围的磁波谱，其中 $R_L$ 是带电粒子的拉莫尔半径。这种能量转移可以阻止磁湍流级联到更小的尺度，导致扩散系数下降，并允许盘和光晕中带电暗物质粒子的有效交换。因此，直接探测实验的地球极限适用于带电暗物质。连同未观察到扩散系数下降，这排除了 $10^2 GeV\lesssim m/q \lesssim 10^{11} GeV$ 的带电暗物质，