  In this work, we report our multi-wavelength observations of the transverse
oscillation of a large scale coronal loop with a length of 350 Mm. The
oscillation was induced by a blowout coronal jet, which was related to a
circular ribbon flare (CRF) in AR 12434 on 2015 October 16. We aim to determine
the physical parameters in the coronal loop, including the Alfven speed and
magnetic field strength. The jet induced kink oscillation was observed in
extreme-ultraviolet (EUV) wavelengths by the Atmospheric Imaging Assembly (AIA)
on board the Solar Dynamics Observatory (SDO). Line of sight magnetograms were
observed by the Helioseismic and Magnetic Imager (HMI) on board SDO. We took
several slices along the loop to assemble time-distance diagrams, and used an
exponentially decaying sine function to fit the decaying oscillation. The
initial amplitude, period, and damping time of kink oscillation were obtained.
Coronal seismology of the kink mode was applied to estimate the Alfven speed
and magnetic field strength in the oscillating loop. In addition, we measured
the magnetic field of the loop through non-linear force free field (NLFFF)
modeling using the flux rope insertion method. The oscillation is most
pronounced in AIA 171 and 131. The oscillation is almost in phase along the
loop with a peak initial amplitude of 13.6 Mm, meaning that the oscillation
belong to the fast standing kink mode. The oscillation lasts for 3.5 cycles
with an average period of 462 s and average damping time of 976 s. The values
of t/P lie in the range of 1.5-2.5. Based on coronal seismology, the Alfven
speed in the oscillating loop is estimated to be 1210 km. Two independent
methods are applied to calculate the magnetic field strength of the loop,
resulting in 30043 G using the coronal seismology and 21123 G using the NLFFF
modeling, respectively.
