that plumes, even though well visible in 2D images beyond the limb, could not be reliably traced to the solar surface. We have reconstructed the 3D geometry of the polar plumes by analysing the simultaneously observed EUVI images for two data sets, April 7 and June 1, 2007. Preliminary results of the 3D plume coordinates obtained on one of the studied days (April 7) are shown in @Curdt:etal:2008. In this paper, we describe an improved method of stereoscopic reconstruction in detail since in @Curdt:etal:2008 the emphasis was put on the multi-spacecraft observations from *Hinode*, *STEREO* and *SOHO*. Furthermore, based on the 3D coordinates, we have calculated the inclination of plumes to the LOS of the Earth and to their local radial direction for both date sets. We have compared the 3D orientation of plumes with the local direction of a dipole magnetic field. The dipole field is the lowest order approximation of the coronal magnetic field at times of low solar activity when the plume observations were made. Additionally, we have calculated the footpoint positions of the reconstructed plumes and projected them onto the EUVI images to investigate their relationship to EUV bright points. For the first data set, *SOHO*/SUMER 