论文标题
在下部太阳大气中由磁重新连接提供动力的白色灯光
A White-light Flare Powered by Magnetic Reconnection in the Lower Solar Atmosphere
论文作者
论文摘要
白光耀斑（WLF）于1859年首次观察到，指的是一种太阳耀斑，显示可见的连续体发射明显增强。这种类型的增强通常发生在大多数能量的耀斑中，通常是由于下部太阳大气中通过非热电子电子从电动机上的能量释放位置向下传播的，因此被解释为有效的加热。但是，这种冠状连接模型难以解释最近发现的小型WLF。在这里，我们报告了与几种观察现象有关的C2.3白光耀斑：相对光电磁通量的快速减小，两个相邻孔消失，下染色体下的较低的染色体的显着加热，硬性X射线磁通量的可忽略不计，以及相关的U型磁场配置。所有这些都表明，这种白光耀斑由太阳大气下部的磁重新连接提供动力，而不是在电晕中更高的重新连接。
White-light flares (WLFs), first observed in 1859, refer to a type of solar flares showing an obvious enhancement of the visible continuum emission. This type of enhancement often occurs in most energetic flares, and is usually interpreted as a consequence of efficient heating in the lower solar atmosphere through non-thermal electrons propagating downward from the energy release site in the corona. However, this coronal-reconnection model has difficulty in explaining the recently discovered small WLFs. Here we report a C2.3 white-light flare, which are associated with several observational phenomena: fast decrease in opposite-polarity photospheric magnetic fluxes, disappearance of two adjacent pores, significant heating of the lower chromosphere, negligible increase of hard X-ray flux, and an associated U-shaped magnetic field configuration. All these suggest that this white-light flare is powered by magnetic reconnection in the lower part of the solar atmosphere rather than by reconnection higher up in the corona.
