Solar flares are sudden and massive releases of magnetic energy in the corona. As a consequence, particles are efficiently accelerated to high energies and plasma is heated up to tens of millions K . However, this phenomenon is dynamically and morphologically complex. A characteristic of this complexity is the creation of multiple acceleration sites due to the magnetic field reconfiguration. During the flare, the energetic electrons propagating in the loops emits in high-frequency radio wavelengths via gyrosyntrochton emission mechanism . Some class of energetic particles may undergo plasma instabilities producing intense coherent radio emission . Accelerated electrons and hot plasma also produce X-ray bremsstrahlung. The heated plasma filling the magnetic loops show up as bright emissions in various extreme ultra-violet (EUV) wavelengths. This entire flare process shows complex evolution at fine spatial, spectral and temporal scales. Therefore, a more comprehensive understanding of solar flares requires multi-wavelength analysis with observations that provide high spatial resolution coupled with high frequency and time resolution.