新兴通量区中普遍存在的细尺度亮点的SolO/EUI观测：与双rost MHD模拟的比较
SolO/EUI Observations of Ubiquitous Fine-scale Bright Dots in an Emerging Flux Region: Comparison with a Bifrost MHD Simulation
摘要：
我们报告了在174光年内用SolO的EUI/ \hri \观测到的一个新兴通量区域（X射线/日冕亮点）内和周围存在许多微小的亮点。这些圆点呈圆形，直径为675 $\pm$ 300 km，寿命为50 $\pm$ 35秒，强度比周围环境高出30 $\pm$ 10%。大约一半的点在其演化过程中保持孤立，并随机缓慢地移动（$<$ 10 \kms）。另一半则表现为扩展，表现为一个小的环或浪涌/喷流，强度传播低于30\，\kms。许多较大且较亮的\hri \点在SDO/AIA 171磁迹通道中可辨别，在1- 2 MK的温度范围内具有显著的发射率，并且通常位于HMI LOS磁图中观察到的极性反转线处。虽然不像观测中那样普遍，但Bifrost MHD模拟的新兴通量区域确实在合成\fe \图像中显示出点。模拟中的这些点显示出明显的多普勒特征--蓝移和红移共存，或者10 \kms \量级的红移之后是类似或更高量级的蓝移。代表过渡区辐射的\oxy \和\siiv \行的合成图像也显示了在\fe \行图像中观察到的点，这些点通常尺寸扩大或延伸为环，并且总是具有比\fe中更强的多普勒速度（高达100 \kms）。我们的观测和模拟结果，以及模拟中的点的场的几何形状，表明大多数点在新兴的通量区形成在较低的太阳大气（在$\approx$ 1 Mm）通过新兴和预先存在/新兴的磁场之间的磁重联。有些斑点可能是磁声冲击通过\fe \发射谱线形成区的表现。
英文摘要：
We report on the presence of numerous tiny bright dots in and around an emerging flux region (an X-ray/coronal bright point) observed with SolO's EUI/\hri\ in 174 Å. These dots are roundish, have a diameter of 675$\pm$300 km, a lifetime of 50$\pm$35 seconds, and an intensity enhancement of 30\% $\pm$10\% above their immediate surroundings. About half of the dots remain isolated during their evolution and move randomly and slowly ($<$10 \kms). The other half show extensions, appearing as a small loop or surge/jet, with intensity propagations below 30\,\kms. Many of the bigger and brighter \hri\ dots are discernible in SDO/AIA 171 Å channel, have significant emissivity in the temperature range of 1--2 MK, and are often located at polarity inversion lines observed in HMI LOS magnetograms. Although not as pervasive as in observations, Bifrost MHD simulation of an emerging flux region do show dots in synthetic \fe\ images. These dots in simulation show distinct Doppler signatures -- blueshifts and redshifts coexist, or a redshift of the order of 10 \kms\ is followed by a blueshift of similar or higher magnitude. The synthetic images of \oxy\ and \siiv\ lines, which represent transition region radiation, also show the dots that are observed in \fe\ images, often expanded in size, or extended as a loop, and always with stronger Doppler velocities (up to 100 \kms) than that in \fe\ lines. Our observation and simulation results, together with the field geometry of dots in the simulation, suggest that most dots in emerging flux regions form in the lower solar atmosphere (at $\approx$1 Mm) by magnetic reconnection between emerging and pre-existing/emerged magnetic field. Some dots might be manifestations of magneto-acoustic shocks through the line formation region of \fe\ emission.
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