The tenuous outer atmosphere of the Sun commonly known as 'corona', is orders of magnitude hotter than the solar surface.

Heating of the solar corona along with acceleration of solar wind remain two of the most puzzling problems in the solar

and space physics. There are several theories proposed to explain the phenomena, however, to identify any one dominant

process is extremely difficult to do. Magnetohydrodynamics (MHD) waves and magnetic reconnection resulting in to transient

release of energy, are currently the most promising heating models. In this presentation, I will mainly discuss different wave

modes possible in the solar corona and their observational signatures. Some recent observational examples of propagation,

and damping of MHD waves in the solar atmosphere will be presented. Contribution of energy carried by these waves in

the context of heating of solar corona and acceleration of solar wind will also be discussed. Few examples of small-scale

transient energy release events due to magnetic reconnection and their importance in the heating of solar atmosphere will

also be presented.