Aims. Recurring jets are observed in the solar atmosphere, which can erupt intermittently. By the observation of intermittent jets, we want to understand the causes of periodic eruption characteristics. Methods. We report intermittent jets observed by the GST. The analysis was aided by 1400 Å and 2796 Å data from IRIS.These observational instruments allowed us to analyze the temporal characteristics of jet events. Results. The jet continued for up to 4 hours. The time distance diagram shows that the peak of the jet has obviously periodic eruption characteristics (5 minutes) during 18:00 UT-18:50 UT. We also found periodic brightening phenomenon (5 minutes) during jets bursts in the observed bands in the Transition Region (1400 Å and 2796 Å), which may be a response to intermittent jets in the upper solar atmosphere.The time lag is 3 minutes. Evolutionary images in the TiO band revealed the horizontal movement of granulation at the location of jet. Compared to the quiet region of the Sun, we found that the footpoint of the jet is enhanced at the center of the H α spectral line profile, with no significant changes in the line wings. This suggests the presence of prolonged heating at the footpoint of the jet. In the mixed-polarity magnetic field region of the jet, we observed magnetic flux emergence, cancellation, and shear indicating possible intermittent magnetic reconnection. That is confirmed by the NLFFF model reconstructed using the magneto-friction method. Conclusions. The multi-wavelength analysis indicates that the events we studied were triggered by magnetic reconnection caused by mixed-polarity magnetic fields. We suggest that the horizontal motion of the granulation in the photosphere drives the magnetic reconnection, which is modulated by p-mode oscillations.
Thin coronal jets and plasmoid-mediated reconnection: Insights from Solar Orbiter observations and Bifrost simulations
Universidad de La Laguna（拉古纳大学）；University of Oslo（奥斯陆大学）；George Mason University（乔治梅森大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Royal Observatory of Belgium（比利时皇家天文台）；KU Leuven（荷语鲁汶大学）
研究结合 Solar Orbiter/HRIEUV 观测与 Bifrost 模拟，识别 CBP 起源的253–706 km细薄日冕喷流，并发现电流片及外流区中等离子体团介导重联的直接与间接证据。
Capturing transient plasma flows and jets in the solar corona
在紫外线（UV）到X射线波长的强度爆发和等离子体喷流是典型的磁重联和相关的脉冲加热的太阳大气等离子体的签名。为了获得新的见解的过程中，高节奏的观测需要捕捉快速响应的等离子体的磁重联以及高度动态的演变射流。在这里，我们报告的第一个2秒的节奏极端紫外线观测记录的174毫米高分辨率成像仪的极紫外线成像仪上的太阳轨道飞行器任务。这些观测覆盖了平静的太阳日冕区域，揭示了磁重联作为局部加热事件的起始特征。这些局部源然后表现出重复的等离子体爆发或喷射活动。我们的观测表明，这种从局部源到喷流活动的空间形态变化可能在大约20秒的时间尺度上迅速发生。喷流本身是间歇性的，从源区产生的时间尺度约为20秒。在这些事件的初始阶段，等离子体射流观察到表现出的速度，从传播强度扰动推断，在100 km s $^{-1}$到150 km s $^{-1}$的范围内。然后，这些射流传播到长度约为5微米。我们讨论的双向和单向射流活动的例子，观察到已开始从最初的本地化爆发在日冕。日冕爆发和相关的等离子体流或喷流的瞬态性质及其动力学可以为日冕爆发和喷流的磁重联模型提供基准。
