Detection and Dynamics of Waves and Flows in the Inner to Middle Solar Corona

The solar corona remains a highly dynamic environment where the coupling between magnetic fields and plasma drives the acceleration of the solar wind and maintains the corona at high termperature. Detection of the propagating disturbances (PD) from the inner to middle corona provides vital clues in the understadning of this subject. Recent advancements in high-resolution imaging and spectroscopy, have enabled the first direct detections of elusive wave modes and fine-scale flows between 1.1 R to 3.6 R. For example, High-cadence observations from the Metis coronagraph on Solar Orbiter have identified pervasive, low-amplitude (0.1% of background) density fluctuations propagating at 150 – 450 km/s up to 2.5 R. High frequency observations has been reported from Fe lines in the corona as well. In this talk I will give a quick overview of recent reports in this field and also highlight the potential of PUNCH and VELC coronagraph observations providing synergies in the understanding of the properties and characteristaion of these PDs.