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Even in quiet areas underneath coronal holes the solar chromosphere containsubiquitous heating events. They tend to be small scale and short lived, hencedifficult to identify. Here we do not address their much-debated contributionto outer-atmosphere heating, but their aftermaths. We performed a statisticalanalysis of high-resolution observations in the Balmer H-alpha line to suggestthat many slender dark H-alpha fibrils spreading out from network representcooling gas that outlines tracks of preceding rapid type II spicule events orsmaller similar but as yet unresolved heating agents in which the main gasconstituent, hydrogen, ionizes at least partially. Subsequent recombinationthen causes dark H-alpha fibrils enhanced by nonequilibrium overopacity. Wesuggest that the extraordinary fibrilar appearance of the H-alpha chromospherearound network results from intermittent, frequent small-scale prior heating.

Solar H-alpha features with hot onsets. IV. Network fibrils