论文标题
C1.7太阳耀斑中高速下流的光谱观测
Spectroscopic Observations of High-speed Downflows in a C1.7 Solar Flare
论文作者
论文摘要
在本文中，我们分析了C1.7太阳耀斑（Sol2017-09-09T06：51）的高分辨率UV光谱，该光谱由\ textIt {接口区域成像光谱}（\ textit {iris {iris}）观察到。 {我们专注于\ ion {si} {4} {4}1402.8Å（$ \ sim $ 10 $^{4.8} $ k）和\ ion {c} {c} {2} {2} 1334.5/1334.5/1335.7Å（$ 10 $ 10 $ 10 $ sim}的位置，速度高达$ \ sim $ 150 km s $^{ - 1} $。}这些红移出现在耀斑的上升阶段，然后迅速增加，在几分钟内达到最大值，然后进入衰减阶段。将来自\ textIt {iris}的图像与大气成像组件（AIA）结合在{\ em solar Dynamics obervatory}（{\ em sdo}）上，我们建议凉线中的红移在过渡区域和上色层中的下降引起，这可能是由磁性重新构成的。此外，在其他一些位置，凉爽的\ ion {si} {4} {4}和\ ion {c} {2}线在其他一些位置显示温和的红移（几十km s $^{ - 1} $），这在上述位置表现出一些独特的特征。这应该来自不同的物理过程。
In this paper, we analyze the high-resolution UV spectra for a C1.7 solar flare (SOL2017-09-09T06:51) observed by the \textit{Interface Region Imaging Spectrograph} (\textit{IRIS}). {We focus on the spectroscopic observations at the locations where the cool lines of \ion{Si}{4} 1402.8 Å ($\sim$10$^{4.8}$ K) and \ion{C}{2} 1334.5/1335.7 Å ($\sim$10$^{4.4}$ K) reveal significant redshifts with Doppler velocities up to $\sim$150 km s$^{-1}$.} These redshifts appear in the rise phase of the flare, then increase rapidly, reach the maximum in a few minutes, and proceed into the decay phase. Combining the images from \textit{IRIS} and Atmospheric Imaging Assembly (AIA) on board the {\em Solar Dynamics Observatory} ({\em SDO}), we propose that the redshifts in the cool lines are caused by the downflows in the transition region and upper chromospheric layers, which likely result from a magnetic reconnection leading to the flare. In addition, the cool \ion{Si}{4} and \ion{C}{2} lines show gentle redshifts (a few tens of km s$^{-1}$) at some other locations, which manifest some distinct features from the above locations. This is supposed to originate from a different physical process.
