  A new mechanism of particle acceleration to ultra high energies, driven by
the rotational slow down of a pulsar (Crab pulsar, for example), is explored.
The rotation, through the time dependent centrifugal force, can very
efficiently excite unstable Langmuir waves in the e-p plasma of the star
magnetosphere via a parametric process. These waves, then, Landau damp on
electrons accelerating them in the process. The net transfer of energy is
optimal when the wave growth and the Landau damping times are comparable and
are both very short compared to the star rotation time. We show, by detailed
calculations, that these are precisely the conditions for the parameters of the
Crab pulsar. This highly efficient route for energy transfer allows the
electrons in the primary beam to be catapulted to multiple TeV ($\sim 100$ TeV)
and even PeV energy domain. It is expected that the proposed mechanism may,
partially, unravel the puzzle of the origin of ultra high energy cosmic ray
electrons.
