Dr. GIRJESH R. GUPTA

One of the most persistent problems in solar physics is the identification of the mechanism that heats the solar corona and accelerates the fast solar wind. Magneto-hydrodynamic (MHD) waves play an important role in heating of the solar corona and acceleration of the fast solar wind. In this presentation, the speaker will mainly focus on coronal hole regions which are relatively cooler and darker regions of solar corona, as observed both on the solar disk and above the solar limb. They are associated with rapidly expanding open magnetic fields and are considered as source region of high-speed solar wind stream. Different types of oscillations have now been observed by various instruments in the solar atmosphere and are interpreted due to ubiquitous presence of MHD waves. Based on observational signatures, identification of various oscillatory and propagating features in the solar corona in terms of different wave modes will be presented.