  We suggest that narrow, long radio filaments near the Galactic Center arise
as kinetic jets - streams of high energy particles escaping from ram-pressure
confined pulsar wind nebulae (PWNe). The reconnection between the PWN and
interstellar magnetic field allows pulsar wind particles to escape, creating
long narrow features. They are the low frequency analogs of kinetic jets seen
around some fast-moving pulsars, such as The Guitar and The Lighthouse PWNe.
The radio filaments trace a population of pulsars also responsible for the
Fermi GeV excess produced by the Inverse Compton scattering by the pulsar wind
particles. The magnetic flux tubes are stretched radially by the large scale
Galactic winds. In addition to PWNe accelerated particles can be injected at
supernovae remnants. The model predicts variations of the structure of the
largest filaments on scales of $\sim$ dozens of years - smaller variations can
occur on shorter time scales. We also encourage targeted observations of the
brightest sections of the filaments and of the related unresolved point sources
in search of the powering PWNe and pulsars.
