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 are proposed to play an important role in the heating of solar corona and acceleration of the fast solar wind. 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. Spectroscopic observations of propagating disturbances are important so as to perform detailed line profile study in order to identify their true nature. Evidence of damping of slow magneto-acoustic waves in the coronal hole will also be presented.