Chromospheric Bubbles in Solar Flares
Chromospheric Bubbles in Solar Flares
复制标题
太阳耀斑中的色球层气泡
DOI：
10.3847/2041-8213/ab8d1e
复制
发表时间：
2020
期刊：
影响因子：
--
通讯作者：
M. Mathioudakis
中科院分区：
文献类型：
--
作者：
A. Reid;B. Zhigulin;M. Carlsson;M. Mathioudakis
我们分析了太阳耀斑的辐射流体动力学模拟网格，以研究大气对非热电电子束加热的能量平衡和响应。色球泡的出现是我们在模拟中发现的最显著的特征之一。这些色球等离子体的口袋被困在过渡区和低层大气之间，因为它被粒子束过热。色球气泡在合成光谱中可以看到，作为巴尔默谱线剖面的附加成分出现，其多普勒速度高达200 km s−1。它们的特征也可以在Ca ii 8542 Å的翼上看到。这些色球等离子体的气泡是由能量沉积冲击引起的波前向上驱动的，需要特定的加热速率和大气位置才能显现。
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.
DOI：
10.3847/1538-4357/aacc29
发表时间：
2018-07
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Stephen Brown;L. Fletcher;G. Kerr;N. Labrosse;A. Kowalski;Jaime de la Cruz Rodr'iguez
通讯作者：
Stephen Brown;L. Fletcher;G. Kerr;N. Labrosse;A. Kowalski;Jaime de la Cruz Rodr'iguez
DOI：
10.3847/0004-637x/827/2/101
发表时间：
2016-05
期刊：
The Astrophysical Journal
影响因子：
--
作者：
G. Kerr;L. Fletcher;A. Russell;J. Allred
通讯作者：
G. Kerr;L. Fletcher;A. Russell;J. Allred