| Abstract : | In this study, we employed two distinct methodologies to estimate magnetic field strengths within coronal loops which are exhibiting transverse oscillations. Our analysis focused on events marked by Transverse Coronal Loop Oscillations (TLOs), utilizing high-resolution data from the Atmospheric Imaging Assembly (AIA) on the Solar Dynamic Observatory (SDO) and the Extreme Ultraviolet Imager (EUVI) on two spacecraft, A (ahead) and B (behind), of the Solar Terrestrial Relations Observatory (STEREO). We initiated our investigation with the precise determination of loop lengths achieved through stereoscopic tracing of coronal structures. Subsequently, through the analysis of time series data, we derived key oscillatory parameters, including amplitude, period, phase, and damping time. The period of oscillations combined with the obtained coronal loop lengths were then utilized in seismological techniques to estimate the average magnetic field within the oscillating coronal loops, resulting in a magnetic field range of 12 G to 146 G in various coronal loops. To validate our findings, we compared them to magnetic field values obtained through the Nonlinear Force-Free Field (NLFFF) extrapolation method. The NLFFF method yielded magnetic field values ranging from 54 G to 187 G. Significantly, both methodologies produced magnetic field values within a reasonable range. Nevertheless, it is essential to note that the magnetic field values extrapolated using the NLFFF method tended to be higher than those derived from coronal seismology. |
