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We carry out a population study of magnetized radio filaments in the Galacticcenter using MeerKAT data by focusing on the spacing between the filaments thatare grouped. The morphology of a sample of 43 groupings containing 174magnetized radio filaments are presented. Many grouped filaments showharp-like, fragmented cometary tail-like, or loop-like structures in contrastto many straight filaments running mainly perpendicular to the Galactic plane.There are many striking examples of a single filament splitting into two prongsat a junction, suggestive of a flow of plasma along the filaments. Spatialvariations in spectral index, brightness, bending and sharpening along thefilaments indicate that they are evolving on a 10^{5-6}-year time scale. Themean spacings between parallel filaments in a given grouping peaks at$\sim16''$. We argue by modeling that the filaments in a grouping all lie onthe same plane and that the groupings are isotropically oriented in 3D space.One candidate for the origin of filamentation is interaction with an obstacle,which could be a compact radio source, before a filament splits and bends intomultiple filaments. In this picture, the obstacle or sets the length scale ofthe separation between the filaments. Another possibility is synchrotroncooling instability occurring in cometary tails formed as a result of theinteraction of cosmic-ray driven Galactic center outflow with obstacles such asstellar winds. In this picture, the mean spacing and the mean width of thefilaments are expected to be a fraction of a parsec, consistent with observedspacing.

Statistical Properties of the Population of the Galactic Center Filaments II: The Spacing Between Filaments