Slow solar wind sources High-resolution observations with a quadrature view
Slow solar wind sources High-resolution observations with a quadrature view
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慢速太阳风源 具有正交视图的高分辨率观测
DOI：
10.1051/0004-6361/202345983
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发表时间：
2023
影响因子：
6.5
通讯作者：
Barczynski K
中科院分区：
文献类型：
--
作者：
Barczynski K
背景缓慢的太阳风的起源仍然是一个悬而未决的问题。一种可能性是活动区边缘的上升流可能会导致缓慢的太阳风。目的我们旨在解释等离子体上升流是如何产生的，是什么机制造成的，以及上升流区的拓扑结构是什么样子。方法我们使用2022年3月30日利用太阳轨道器上的极紫外成像仪/高分辨率成像仪获得的具有前所未有的时间(3 S)和空间(2像素=236公里)分辨率的成像数据来研究上升流区。在此期间，地球动力学观测站和地球轨道卫星(太阳动力学观测站、日诺德和界面区域成像光谱仪)处于正交位置(∼92°)，这提供了高分辨率的立体图像。我们利用Hinode/EIS(Fe XII)光谱数据在活动区找到了日冕上流区。IRIS狭缝颌部成像仪提供了过渡区和色球的高分辨率图像。结果首次有数据提供了高空间分辨率的日冕上升流区的正交图。我们发现了植根于日冕上升流区的延长环路。通过多普勒频移光谱确定的扩展环的足部的等离子体上升流类似于通过正交成像所看到的明显上升运动。上升流区小尺度结构的动力学可以用来识别等离子体上升流的两种机制：机制I是热冕环与日冕开放磁力线的重联，机制II是色球小环与色球或过渡区开放磁力线的重联。我们确定了机制I和II发挥作用的位置。
ContextThe origin of the slow solar wind is still an open issue. One possibility that has been suggested is that upflows at the edge of an active region can contribute to the slow solar wind.AimsWe aim to explain how the plasma upflows are generated, which mechanisms are responsible for them, and what the upflow region topology looks like.MethodsWe investigated an upflow region using imaging data with the unprecedented temporal (3 s) and spatial (2 pixels = 236 km) resolution that were obtained on 30 March 2022 with the 174 Å channel of the Extreme-Ultraviolet Imager (EUI)/High Resolution Imager (HRI) on board Solar Orbiter. During this time, the EUI and Earth-orbiting satellites (Solar Dynamics Observatory, Hinode, and the Interface Region Imaging Spectrograph, IRIS) were located in quadrature (∼92°), which provides a stereoscopic view with high resolution. We used the Hinode/EIS (Fe XII) spectroscopic data to find coronal upflow regions in the active region. The IRIS slit-jaw imager provides a high-resolution view of the transition region and chromosphere.ResultsFor the first time, we have data that provide a quadrature view of a coronal upflow region with high spatial resolution. We found extended loops rooted in a coronal upflow region. Plasma upflows at the footpoints of extended loops determined spectroscopically through the Doppler shift are similar to the apparent upward motions seen through imaging in quadrature. The dynamics of small-scale structures in the upflow region can be used to identify two mechanisms of the plasma upflow: Mechanism I is reconnection of the hot coronal loops with open magnetic field lines in the solar corona, and mechanism II is reconnection of the small chromospheric loops with open magnetic field lines in the chromosphere or transition region. We identified the locations in which mechanisms I and II work.