We present the morphological and kinematic characteristics of three small-scale X-ray/EUV jets simultaneously observed by the Hinode XRT and the TRACE. For this, we examined all XRT movies with a thin Al/Poly filter from 2006 October 20 to 2007 April 8, and then found 34 small-scale eruptions. We next took a look at the corresponding TRACE 171/195 Å images associated with the eruptions. As a result, we found three simultaneous X-ray and EUV jets. For two different bands, they have similar characteristics in terms of the projected speed (90–310 km s$^{-1}$), lifetime (100–2000 s), and size (1.1–5$\times$10$^5$km). These characteristics are similar to the previous results by the Yohkoh SXT, but are quite different from EUV jets associated with H$\alpha$ surges. From the EUV Imaging Spectrometer, four spectral lines for the last event, we found blueshift (up to $-$64 km s$^{-1}$) and redshift (up to 20 km s$^{-1}$) motions as well as nonthermal velocities ranging from 57 to 106 km s$^{-1}$ at the jet footpoint. We note a tendency: the hotter the maximum ionization temperature is, the smaller the area of blueshift region is. These characteristics are consistent with a typical jet model that includes the magnetic reconnection between open coronal fields and emerging magnetic fields.

We report on the successive occurrence of 0.″5 wide photospheric vortices with strong transverse shear flows at the edge of a sunspot light bridge (LB), and the subsequent ejection of chromospheric surges observed using a Visible Inteferometry Spectrograph, a broadband TiO filter, and a Near InfRared Imaging Spectrograph of the Goode Solar Telescope operating at Big Bear Solar Observatory. The Hα surges ejected at the location of the vortices often appeared in a hollow cylindrical structure. We also observed quasi-periodic vortex-associated bright Hα plasma blobs moving upward with a speed of up to 4 km s−1. In view of the strong shear flow at the edge of the LB, it is likely that the vortices form under the Kelvin–Helmholtz instability. The surges may result from either the magnetic tension generated after magnetic reconnection or an acoustic impulse of a fast photospheric transverse flow. Otherwise, the surges could also be associated with Alfvénic waves, in which case their origin could be torsional magnetic fields generated in the process of the vortex formation.

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We report three-minute oscillations in the solar chromosphere driven by a strong downflow event in a sunspot. We used the Fast Imaging Solar Spectrograph of the 1.6 m New Solar Telescope and the Interface Region Imaging Spectrograph (IRIS). The strong downflow event is identified in the chromospheric and transition region lines above the sunspot umbra. After the event, oscillations occur at the same region. The amplitude of the Doppler velocity oscillations is 2 km s −1 , and gradually decreases with time. In addition, the period of the oscillations gradually increases from 2.7 minutes to 3.3 minutes. In the IRIS 1330 slit-jaw images, we identify a transient brightening near the footpoint of the downflow detected in the Hα+0.5Å image. The characteristics of the downflowing material are consistent with those of sunspot plumes. Based on our findings, we suggest that the gravitationally stratified atmosphere came to oscillate with three minute period in response to the impulsive downflow event as was theoretically investigated by Chae & Goode (2015).

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