Abstarct: Solar wind is a supersonic and super-Alfvenic plasma flow of solar origin which continuously expands into the heliosphere. This medium is the best opportunity to study directly collisionless plasma phenomena.During its expansion, the solar wind develops a strong turbulent character, which evolves towards a state that resembles the well known hydrodynamic turbulence described by Kolmogorov (1941). Because of the presence of a strong magnetic field carried by the wind, low-frequency fluctuations in the solar wind are usually described within a magnetohydrodynamic (MHD). In the limit of high Reynolds number the turbulence is said to be in a fully developed turbulent state. Space plasma like solar wind is fully developed turbulent system. Spectral properties of magnetohydrodynamic turbulence described by Probability Distribution Function and Structure Function. We investigate the the occurrence of intermittency in plasma turbulence by studying the departure from the Gaussian distribution of PDF for magnetic fluctuations. We investigate scaling properties of magnetic field and energy densities.