We analyze a grid of radiative hydrodynamic simulations of solar flares to study the energy balance and response of the atmosphere to nonthermal electron beam heating. The appearance of chromospheric bubbles is one of the most notable features that we find in the simulations. These pockets of chromospheric plasma get trapped between the transition region and the lower atmosphere as it is superheated by the particle beam. The chromospheric bubbles are seen in the synthetic spectra, appearing as an additional component to Balmer line profiles with high Doppler velocities as high as 200 km s −1 . Their signatures are also visible in the wings of Ca ii 8542 Å line profiles. These bubbles of chromospheric plasma are driven upward by a wave front that is induced by the shock of energy deposition, and require a specific heating rate and atmospheric location to manifest.

中文翻译：

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太阳耀斑中的大气层气泡

我们分析了太阳耀斑的辐射流体动力学模拟网格，以研究能量平衡和大气对非热电子束加热的响应。色球气泡的出现是我们在模拟中发现的最显着特征之一。当色球层等离子被粒子束过热时，它们会陷入过渡区和低层大气之间。在合成光谱中可以看到色球泡沫，它是具有高达200 km s -1的高多普勒速度的巴尔默线剖面的附加成分。在Ca ii 8542Å线轮廓的机翼中也可以看到它们的签名。色球层等离子的这些气泡是由能量沉积的震动引起的波阵面向上驱动的，