Probing solar flare accelerated electron distributions with prospective X-ray polarimetry missions
Probing solar flare accelerated electron distributions with prospective X-ray polarimetry missions
复制标题
通过前瞻性 X 射线偏振测量任务探测太阳耀斑加速电子分布
DOI：
10.1051/0004-6361/202038626
复制
发表时间：
2020
影响因子：
6.5
通讯作者：
E. P. Kontar
中科院分区：
文献类型：
--
作者：
N. Jeffrey;P. Saint;E. P. Kontar
太阳耀斑电子加速是一个极其高效的过程，但加速的方法并没有很好的约束。电子各向异性（与引导磁场的速度角）和高能截止（加速条件产生的最高能量电子：机制、空间范围和时间）是两个基本诊断，是有助于限制太阳电子加速的重要物理量，但两者都很难确定。在这里，通过使用电子和 X 射线传输模拟来解释碰撞和非碰撞传输过程，例如湍流散射和 X 射线反照率，我们表明 X 射线偏振可用于约束加速电子分布和最高能加速电子的各向异性。此外，我们表明，前瞻性任务，例如没有成像信息的立方体卫星任务，可以与此类模拟一起使用来确定这些参数。我们的结论是，对耀斑加速过程的更全面了解将来自能够同时进行 X 射线通量和偏振光谱测量的任务。尽管成像偏振测定法是非常理想的，但我们证明不带成像的分光偏振计也可以对电子各向异性和高能量截止提供严格的限制。
Solar flare electron acceleration is an extremely efficient process, but the method of acceleration is not well constrained. Two of the essential diagnostics, electron anisotropy (velocity angle to the guiding magnetic field) and the high energy cutoff (highest energy electrons produced by the acceleration conditions: mechanism, spatial extent, and time), are important quantities that can help to constrain electron acceleration at the Sun but both are poorly determined. Here, by using electron and X-ray transport simulations that account for both collisional and non-collisional transport processes, such as turbulent scattering and X-ray albedo, we show that X-ray polarization can be used to constrain the anisotropy of the accelerated electron distribution and the most energetic accelerated electrons together. Moreover, we show that prospective missions, for example CubeSat missions without imaging information, can be used alongside such simulations to determine these parameters. We conclude that a fuller understanding of flare acceleration processes will come from missions capable of both X-ray flux and polarization spectral measurements together. Although imaging polarimetry is highly desired, we demonstrate that spectro-polarimeters without imaging can also provide strong constraints on electron anisotropy and the high energy cutoff.
影响因子：
4.9
作者：
Aschwanden, Markus J.;Caspi, Amir;Xu, Yan
通讯作者：
Xu, Yan
影响因子：
4.9
作者：
Gary, Dale E.;Chen, Bin;Yu, Sijie
通讯作者：
Yu, Sijie