Institution(s): 1. Yunnan Observatories, Chinese Academy of Sciences
Large amplitude prominence (filament) oscillations could be classified into two categories: the transverse and the longitudinal oscillations. Previous observations indicated that the former type is often trigger by chromosphere Moreton waves in association with remote flares, while the latter is usually associated with nearby micro flare, filament, and jet activities . Using the high temporal and spatial resolution data taken by the SDO, STEREO, and SMART, we present two cases of prominence/filament oscillations induced by large-scale coronal shock waves. For the first case, a chain of oscillating filaments are observed in a proper order after the shock wave associated with a remote X2.1 flare on September 06, 2011, and the filament oscillations were triggered by the surface component of the EUV wave associated with the flare. For the second case, simultaneous transverse oscillation of a limb prominence and longitudinal oscillation in an on-disk filament are launched by the shock wave in association with the X6.9 flare on August 09, 2011. In these observations, the parameters of the oscillating filaments are determined, and they are used to estimate the filament magnetic field. These observations provide new evidence for diagnosing the properties of the oscillating filaments and the associated coronal shock waves.