  A set of 23 observations of coronal jet events that occurred in coronal
bright points has been analyzed. The focus was on the temporal evolution of the
mean brightness before and during coronal jet events. In the absolute majority
of the cases either single or recurrent coronal jets were preceded by slight
precursor disturbances observed in the mean intensity curves. The key
conclusion is that we were able to detect quasi-periodical oscillations with
characteristic periods from sub-minute up to 3-4 min values in the bright point
brightness which precede the jets. Our basic claim is that along with the
conventionally accepted scenario of bright point evolution through new magnetic
flux emergence and its reconnection with the initial structure of the bright
point and the coronal hole, certain MHD oscillatory and wave-like motions can
be excited and these can take an important place in the observed dynamics.
These quasi-oscillatory phenomena might play the role of links between
different epochs of the coronal jet ignition and evolution. They can be an
indication of the MHD wave excitation processes due to the system entropy
variations, density variations or shear flows. It is very likely a sharp
outflow velocity transverse gradients at the edges between the open and closed
field line regions. We suppose that magnetic reconnections can be the source of
MHD waves due to impulsive generation or rapid temperature variations, and
shear flow driven nonmodel MHD wave evolution (self-heating and/or
overreflection mechanisms).
