High-quality imaging spectroscopy in the H{alpha} line, obtained with the CRisp Imaging SpectroPolarimeter (CRISP) at the Swedish 1-m Solar Telescope (SST) at La Palma and covering a small sunspot and its surroundings, are studied. They exhibit ubiqu
itous flows both along fibrils making up the chromospheric canopy away from the spot and in the superpenumbra. We term these flows flocculent to describe their intermittent character, that is morphologically reminiscent of coronal rain. The flocculent flows are investigated further in order to determine their dynamic and morphological properties. For the measurement of their characteristic velocities, accelerations and sizes, we employ a new versatile analysis tool, the CRisp SPectral EXplorer (CRISPEX), which we describe in detail. Absolute velocities on the order of 7.2-82.4 km/s are found, with an average value of 36.5pm5.9 km/s and slightly higher typical velocities for features moving towards the sunspot than away. These velocities are much higher than those determined from the shift of the line core, which shows patches around the sunspot with velocity enhancements of up to 10-15 km/s (both red- and blueshifted). Accelerations are determined for a subsample of features, that show clear accelerating or decelerating behavior, yielding an average of 270pm63 m/s^2 and 149pm63 m/s^2 for accelerating and decelerating features, respectively. Typical flocculent features measure 627pm44 km in length and 304pm30 km in width. On average 68 features are detected per minute, with an average lifetime of 67.7pm8.8 s. The dynamics and phenomenology of the flocculent flows suggest they may be driven by a siphon flow, where the flocculence could arise from a density perturbation close to one of the footpoints or along the loop structure.
High-resolution imaging-spectroscopy movies of solar active region NOAA 10998 obtained with the CRisp Imaging SpectroPolarimeter (CRISP) at the Swedish 1-m Solar Telescope show very bright, rapidly flickering, flame-like features that appear intermit
tently in the wings of the Balmer H-alpha line in a region with moat flows and likely some flux emergence. They show up at regular H-alpha blue-wing bright points that outline magnetic network, but flare upward with much larger brightness and distinct jet morphology seen from aside in the limbward view of these movies. We classify these features as Ellerman bombs and present a morphological study of their appearance at the unprecedented spatial, temporal, and spectral resolution of these observations. The bombs appear along magnetic network with footpoint extents up to 900km. They show apparent travel away from the spot along the pre-existing network at speeds of about 1 km/s. The bombs flare repetitively with much rapid variation at time scales of seconds only, in the form of upward jet-shaped brightness features. These reach heights of 600-1200km and tend to show blueshifts; some show bi-directional Doppler signature, and some seem accompanied with an H-alpha surge. They are not seen in the core of H-alpha due to shielding by overlying chromospheric fibrils. The network where they originate has normal properties. The morphology of these jets strongly supports deep-seated photospheric reconnection of emergent or moat-driven magnetic flux with pre-existing strong vertical network fields as the mechanism underlying the Ellerman bomb phenomenon.
