  A Crescent shaped prominence Structure (CS), over the solar west limb is
studied using EIS/HINODE and AIA/SDO. First, the time varying positions of the
top and below borders of the CS, along with its central axis are derived. Time
evolutions of the Doppler shifts, and Line width of Fe~{\scriptsize \rm XII}
195.119 line are studied over the CS borders. Transverse kink oscillations are
observed both in the Solar-Y direction and in the Doppler shifts over the
observers' LOS. One explanation could be the oscillatory direction of the main
kink wave build an angle with the observers LOS. This angle is calculated to be
equal to 27 degrees for the CS top border. The main kink amplitude velocity and
periods are obtained to be 5.3 $\rm km/s$, and 33.4 minutes, respectively. The
anti-correlation observed between the brightness and thickness of the CS (with
-178.1$^\circ$) suggests the presence of sausage modes with periods of 20.8
minutes. Based on the AIA imaging, it is suggested that the occurred jets and
their afterward dimming are responsible to trigger the sausage mode. The
average electron densities of the CS over the time of the study is obtained to
be log($\rm n_e$)=9.3$\rm [cm^{-3}]$. The Alfv\'en velocity, magnetic field,
and energy flux of the observed fast kink mode over the CS are estimated to be
16.7 $\rm km/s$, 2.79 $\rm G$, 41.93 $\rm W/m^2$. Considering the magnetic flux
conservation inside the CS, expanding the CS cross section, causes the magnetic
field to decay with the rate of $\rm 4.95 \times 10^{-4} \, G/sec$.
