  Observational evidence shows that coronal jets can hit prominences and set
them in motion. The impact leads to large-amplitude oscillations (LAOs) of the
prominence. In this paper we attempt to understand this process via 2.5D MHD
numerical experiments. In our model, the jets are generated in a sheared
magnetic arcade above a parasitic bipolar region located in one of the
footpoints of the filament channel (FC) supporting the prominence. The shear is
imposed with velocities not far above observed photospheric values; it leads to
a multiple reconnection process, as in previous jet models. Both a fast
Alfv\'enic perturbation and a slower supersonic front preceding a plasma jet
are issued from the reconnection site; in the later phase, a more violent
(eruptive) jet is produced. The perturbation and jets run along the FC; they
are partially reflected at the prominence and partially transmitted through it.
There results a pattern of counter-streaming flows along the FC and
oscillations of the prominence. The oscillations are LAOs (with amplitude above
$10~\mathrm{km\, s^{-1}}$) in parts of the prominence both in the longitudinal
and transverse directions. In some field lines, the impact is so strong that
the prominence mass is brought out of the dip and down to the chromosphere
along the FC. Two cases are studied with different heights of the arcade above
the parasitic bipolar region, leading to different heights for the region of
the prominence perturbed by the jets. The obtained oscillation amplitudes and
periods are in general agreement with the observations.
