Abstract Details


Name: Safna Banu K
Affiliation: NIT Calicut
Conference ID: TVS202510208
Title: Fundamental and Overton Transverse Coronal Loop Oscillations for Coronal Seismological Applications
Authors and Co-Authors:
Abstract Type: Contributory Presentation
Abstract: A dynamic environment, the solar corona contains a variety of magnetic structures, such as holes, plumes, and coronal loops. Dynamic activity like flares, CMEs, and magnetohydrodynamic waves disturbs these structures, causing oscillations that can be used as a proxy for studying the characteristics of the solar corona. The fundamental modes and overtones in the transverse oscillations of coronal loops linked to an active region are identified in this work. We examine intensity data from the Solar Dynamics Observatory's (SDO)/ Atmospheric Imaging Assembly (AIA) and Extreme Ultraviolet Imager (EUVI) from Solar-Terrestrial Relation Observatory (STEREO). Fundamental oscillation periods of roughly 17.0 minutes for the first loop and 15.2 minutes for the second loop are shown by our analysis. The first and second overtones of the first coronal loop show oscillations with periods of 6.9 and 4.3 minutes, respectively. On the other hand, only the first overtone, which has a duration of almost 7.7 minutes, contained the second loop. These loops have fundamental to first overtone period ratios of 1.24 and 0.99, respectively, but the first loop has a fundamental to second overtone ratio of 1.33. These period ratio departures from unity offer important information for calculating the density scale height and loop expansion factor. According to our findings, the first loop's loop expansion factor is 1.5, and the second loop's density scale height is 11 Mm. This implies that coronal loop characteristics have a greater impact on the loop expansion factor than the longitudinal density stratification usually found in sigmoidal active regions. Furthermore, we calculated the average magnetic field strength within the coronal loops to be between 20 and 30 G by comparing their lengths with their oscillation times. We also report statistical analyses that use coronal seismology and extrapolation methods to assess the consistency of magnetic field observations.