Waves and oscillations are pervasive throughout the solar atmosphere, serving as vital diagnostic signatures when interpreted through the framework of Magnetohydrodynamic (MHD) theory. This thesis investigates the physical properties of the solar atmosphere through a multi-scale seismological approach, progressing from high-frequency wave dynamics to long-period oscillations. We begin by utilizing high spatial and temporal resolution observations from the Solar Orbiter’s Extreme Ultraviolet Imager (EUI) to probe the high-frequency oscillations in polar plumes, where we report the simultaneous detection of slow magneto-acoustic waves and kink waves with periodicities of 100 seconds. These high-resolution observations allow us to resolve fine-scale substructures within the polar plumes. Transitioning to the 5-minute oscillation regime, we employ Coronal Multichannel Polarimeter (CoMP) data to obtain a global map of the coronal magnetic field. By applying Bayesian inference to ubiquitous kink waves, we demonstrate that probabilistic methods provide better constraints on magnetic field strength compared to simple inversion. Finally, we address the long-period regime by analyzing simultaneous longitudinal and transverse oscillations in quiescent solar prominences. Using the Bayesian framework, we infer the magnetic field strength and subsequently constrain the geometry of the supporting magnetic flux tubes, revealing lengths ranging from 100 to 1000 Mm and low twist numbers. Collectively, these results demonstrate that high-resolution observations of fine-scale dynamics and Bayesian seismology of large-scale oscillations offer a comprehensive diagnostic framework, enabling precise constraints on the plasma properties of the solar corona.