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Cool-core clusters (e.g., Perseus or M87) often possess a network of brightgaseous filaments, observed in radio, infrared, optical and X-ray bands. Wepropose that these filaments are powered by the reconnection of the magneticfield in the wakes of buoyant bubbles. AGN-inflated bubbles of relativisticplasma rise buoyantly in the cluster atmosphere, stretching and amplifying thefield in the wake to values of $\displaystyle \beta =8\pi P_{gas}/B^2\sim 1$.The field lines in the wake have opposite directions and are forced together asthe bubble motion stretches the filament. This setup bears strong similarity tothe coronal loops on the Sun or to the Earth's magneto-tail. The reconnectionprocess naturally explains both the required level of local dissipation rate infilaments and the overall luminosity of filaments. The original source of powerfor the filaments is the potential energy of buoyant bubbles, inflated by thecentral AGN.

Powering of cool filaments in cluster cores by buoyant bubbles. I. Qualitative model