光学氢谱线对束流加热的响应：I.电子束
Response of optical hydrogen lines to beam heating: I. Electron beams
摘要：
我们调查的作用，非热电子的形成区域的H α，H β，和H γ线，以展开他们的影响，这些线的形成。我们专注于脉冲束加热在亚秒级的时间尺度上变化。此外，我们从理论上探讨了一种新的诊断工具存在的可能性，表明存在的非热电子在耀斑色球光学氢线的基础上的观测。为了模拟燃烧的大气和随时间变化的氢的激发和电离的演变，我们使用了1-D辐射流体动力学代码相结合的测试粒子代码，模拟的传播，散射，和热化的幂律电子束，以获得耀斑加热和非热碰撞率由于光束与氢原子的相互作用。所有计算的模型都显示了亚秒级时间尺度上的模拟巴耳末线强度的时间相关响应，与亚秒级的光束通量后面的时滞。取决于光束参数，线中心和翼都可以显示出明显的强度变化。非热碰撞率通常导致色球层中形成的次级区域的发射增加。
英文摘要：
We investigate the role of non-thermal electrons in the formation regions of Halpha, Hbeta, and Hgamma lines in order to unfold their influence on the formation of these lines. We concentrate on pulse-beam heating varying on a subsecond timescale. Furthermore, we theoretically explore possibility that a new diagnostic tool exists indicating the presence of non-thermal electrons in the flaring chromosphere based on observations of optical hydrogen lines. To model the evolution of the flaring atmosphere and the time-dependent hydrogen excitation and ionisation, we used a 1-D radiative hydrodynamic code combined with a test-particle code that simulates the propagation, scattering, and thermalisation of a power-law electron beam in order to obtain the flare heating and the non-thermal collisional rates due to the interaction of the beam with the hydrogen atoms. All calculated models have shown a time-correlated response of the modelled Balmer line intensities on a subsecond timescale, with a subsecond timelag behind the beam flux. Depending on the beam parameters, both line centres and wings can show pronounced intensity variations. The non-thermal collisional rates generally result in an increased emission from a secondary region formed in the chromosphere.
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