Top panel: coordinated multiwavelength observations of two QSEBs (labeled as colored 1 and 2 in the lower panel of Figure 1) spanning from the lower to upper solar atmosphere, including Fe I 6302 Å wing, Stoke V of Fe I 6302 Å, Hα wing, Ca II 8542 Å wing, Hβ wing, Ca II K wing, IRIS SJI 2832 Å, 2796 Å, 1400 Å, and SDO/AIA 1600 Å, 1700 Å, 304 Å, 131 Å, 171 Å, 193 Å, and 211 Å channels. Bottom panel: spectral profiles at the QSEB locations in Hα, Hβ,Ca II 8542 Å, and Ca II H and K. Red and blue lines represent EB and quiet-Sun spectra, respectively, while green and magenta lines show the difference (QSEB minus quiet Sun) and the normalized zero level. The spectra exhibit typical wing enhancements characteristic of QSEBs. Although QSEBs are observed nearly cospatially and cotemporally in chromospheric wings and IRIS SJIs, and AIA 1600/1700 Å channels, they remain undetected in hotter AIA channels. The animation spans a total duration of ∼1 s and consists of 9 frames for QSEB-1 and 15 frames for QSEB-2, illustrating the temporal evolution of the QSEBs in the Hβ spectral line.

(An animation of this figure is available in the online article.)

(An animation of this figure is available.)

The video/animation of this figure is available in the online journal.