Abstract:
The fast solar wind originates from polar coronal holes. Recent observations from SoHO suggest that the solar wind is flowing from funnel-shaped magnetic fields anchored in the lanes of the magnetic network at the solar surface. Using the spectroscopic diagnostic capability of SUMER on SoHO and of EIS on HINODE, we study waves in polar coronal holes, in particular their origin, nature, and acceleration. The variation of the width of spectral lines with height above the solar surface supplies information on the properties of waves as they propagate out of the Sun.
