AI 中文总结
本研究利用 DKIST 高分辨率观测，发现 Hβ 针状体、小尺度喷流和微闪等亚角秒色球层瞬变事件源于磁重联，携带足够能量加热色球层和日冕，对太阳风加速有潜在贡献。
AI 中文摘要
我们利用丹尼尔·井上太阳望远镜（DKIST）的可见光宽带成像仪（VBI）获取的 Hβ 图像以及 DKIST 可见光谱偏振仪（ViSP）获取的视向磁图，研究了太阳盘面上一个增强磁网络区域的宁静区。我们还将 ViSP 磁图与太阳动力学天文台（SDO）/日震与磁成像仪（HMI）获取的共对准、同时刻的视向磁图进行了比较。我们发现：（i）存在两类色球层喷流状特征：Hβ 针状体和小尺度喷流。两者均根植于磁网络通道边缘附近。其中若干喷流靠近 ViSP 探测到的少数极性磁通小岛或多数极性磁通中的凹陷区域。因此，这些喷流可能源于混合极性磁通，并由色球层磁重联引起。对于 Hβ 针状体，其平均宽度、长度、寿命和速度分别为 420±400 km、2600±1600 km、4.3±0.25 分钟和 12±4.7 km/s。对于小尺度喷流，这些参数分别为 385±100 km、620±40 km、5±3 分钟和 4.4±1.5 km/s。（ii）Hβ 微闪位于明显的单极性磁通区域。其宽度、长度、寿命和速度分别为 180±65 km、365±100 km、4.3±2.6 分钟和 3.1±0.2 km/s。（iii）在日冕羽流底部，由于 ViSP 的空间分辨率高于 HMI，ViSP 显示了一些 HMI 未显示的很强（>800 G）的多数极性磁通，以及一些 HMI 未显示的亚角秒少数极性磁通夹杂物。这些亚角秒色球层瞬变事件携带足够的能量（10^24 尔格），可瞬态加热局部色球层和日冕，并可能对太阳风加速做出贡献。它们可能代表了磁重联驱动活动连续谱中的小尺度端，凸显了 DKIST 高分辨率磁场测量对于理解小尺度色球层动力学的重要性。
英文摘要
We examine an on-disk solar quiet region of enhanced magnetic network using Hbeta images from Daniel K. Inouye Solar Telescopes (DKISTs) Visible Broadband Imager (VBI) and line-of-sight magnetograms from DKISTs Visible Spectro-Polarimeter (ViSP). We also compare the ViSP magnetograms with co-aligned co-temporal line-of-sight magnetograms from the Solar Dynamics Observatory (SDO)/Helioseismic and Magnetic Imager (HMI). We find:(i) Two types of chromospheric jet-like features: Hbeta spicules, and small-scale jets. Both are rooted near edges of magnetic network lanes. Several sit close to ViSP-detected tiny islands of either minority-polarity flux or dips in majority-polarity flux. Hence, those several plausibly stem from mixed-polarity magnetic flux, and are caused by chromospheric magnetic reconnection. For H\b{eta} spicules, the average width, length, lifetimes, and speeds are 420$\pm$400 km, 2600$\pm$1600 km, 4.3$\pm$0.25 min, and 12$\pm$4.7 kms. For small-scale jets, those are 385$\pm$100 km, 620$\pm$40 km, 5$\pm$3min, and 4.4$\pm$1.5 kms. (ii) H$β$ microflashes sit in evidently unipolar flux. Their widths, lengths, lifetimes, and speeds are 180$\pm$65 km, 365$\pm$100 km, 4.3$\pm$2.6 min, and 3.1$\pm$0.2 kms. (iii) At the base of a coronal plume, due to its higher spatial resolution than HMI, ViSP shows both some very strong (>800 G) majority-polarity flux not shown by HMI and some sub-arc-second minority-polarity-flux inclusions not shown by HMI. These sub-arcsecond chromospheric transients carry sufficient energy (10^{24}erg) to transiently heat the local chromosphere and corona and potentially contribute to solar-wind acceleration. They may represent the small-scale end of a continuum of magnetic-reconnection-driven activity, highlighting the importance of DKIST's high-resolution magnetic-field measurements for understanding small-scale chromospheric dynamics.
Comments17 pages, 9 figures, 1 table, accepted for publication in ApJ Letters
