Waves and turbulence in the solar wind

It is now believed that magnetohydrodynamics (MHD) provides an ideal description for the solar wind. Waves, observed via remote sensing and detected in-situ in the wind streams, are most likely responsible for the wind. The detection of these waves in the outer solar atmosphere is made possible by analysing the effects these waves have on the plasma. The presence or signature of compressional waves may be seen in the form of variations or oscillations in radiance, due to change in plasma density, and also in the line-of-sight (LOS) velocities, due to plasma motions. On the other hand, transverse waves keep their signature in the broadening of spectral lines. I will review the status of the detection of these waves through imaging and spectroscopic methods. Finally I will present few theoretical models which describe the role of MHD waves in the acceleration of the fast solar wind.