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

Transverse oscillation of a coronal loop induced by a flare-related jet