Physical properties of a fan-shaped jet backlit by an X9.3 flare
Physical properties of a fan-shaped jet backlit by an X9.3 flare
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X9.3 耀斑背光扇形射流的物理特性
DOI：
10.1051/0004-6361/202142346
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发表时间：
2022
影响因子：
6.5
通讯作者：
Pietrow A
中科院分区：
文献类型：
--
作者：
Pietrow A
扇形射流有时在光桥上方形成，被认为是由垂直本影场与光桥上方水平场的重新连接所驱动的。因为这些喷流在大多数色球谱线的翅膀上并不是完全不透明的，所以如果不高度复杂地考虑风扇后面的大气在谱线中的辐射传输，就不可能研究它们的光谱。目的利用瑞典1米太阳望远镜的CRISP和CHROMIS仪器获得的一组独特的h α线以及Ca II 8542 Å和Ca II K线的观测资料，研究X9.3耀斑背光下扇形射流的物理性质。对于我们认为是第一次，我们报告了对扇形射流中物质的质量和密度的观测得出的估计。方法扇后的h α耀斑带发射谱线被高度加宽和平坦化，这使得我们可以通过Beckers云模型来研究扇的单板，就好像它被连续发射的平坦谱线背光一样。利用这个模型，我们推导出了材料在射流中的不透明度和速度。通过斯德哥尔摩反演代码对Ca II 8542 Å的发射进行反演，我们还能够估计温度并交叉检查射流中材料的速度。最后，我们使用质量、平面速度和视距速度作为时间的函数来研究在这个喷流崩溃时向下提供给光球的能量和动量，并评估它是否可能驱动下面的地震。结果风扇材料的物理性质为色球性质，温度为7050±250 K，平均密度为2±0.3 × 10−11g cm−3。结论h α观测到的总质量为3.9±0.7 × 1013g，崩塌时传递到扇底的动能比典型地震能量低近2个数量级。因此，我们排除了这种射流作为地震驱动因素的可能性，但不能完全排除更大的风扇射流作为潜在驱动因素的可能性。
ContextFan-shaped jets sometimes form above light bridges and are believed to be driven by the reconnection of the vertical umbral field with the more horizontal field above the light bridges. Because these jets are not fully opaque in the wings of most chromospheric lines, it is not possible to study their spectra without highly complex considerations of radiative transfer in spectral lines from the atmosphere behind the fan.AimsWe take advantage of a unique set of observations of the Hαline along with the Ca II 8542 Å and Ca II K lines obtained with the CRISP and CHROMIS instrument of the Swedish 1-m Solar Telescope to study the physical properties of a fan-shaped jet that was backlit by an X9.3 flare. For what we believe to be the first time, we report an observationally derived estimate of the mass and density of material in a fan-shaped jet.MethodsThe Hαflare ribbon emission profiles from behind the fan are highly broadened and flattened, allowing us to investigate the fan with a single slab via Beckers’ cloud model, as if it were backlit by a flat spectral profile of continuum emission. Using this model we derived the opacity and velocity of the material in the jet. Using inversions of Ca II 8542 Å emission via the STockholm inversion Code, we were also able to estimate the temperature and to cross-check the velocity of the material in the jet. Finally, we used the masses and the plane-of-sky and line-of-sight velocities as functions of time to investigate the downward supply of energy and momentum to the photosphere in the collapse of this jet, and evaluated it as a potential driver for a sunquake beneath.ResultsWe find that the physical properties of the fan material are reasonably chromospheric in nature, with a temperature of 7050 ± 250 K and a mean density of 2 ± 0.3 × 10−11g cm−3.ConclusionsThe total mass observed in Hαwas found to be 3.9 ± 0.7 × 1013g and the kinetic energy delivered to the base of the fan in its collapse was nearly two orders of magnitude below typical sunquake energies. We therefore rule out this jet as the sunquake driver, but cannot completely rule out larger fan jets as potential drivers.
1980年加拿大西安大略大学太阳能利用国际研讨会
DOI：
--
发表时间：
1980
期刊：
影响因子：
--
作者：
정현채
通讯作者：
정현채