is rather small with an average of $6.47^{\circ}$. The deviation of the plume projection onto the local meridian plane from the local radial direction becomes larger in general with increasing distance of the plume from solar poles. For these two data sets, a simple dipole model with its axis along the solar rotation axis for the global magnetic field does, however, not provide a good description of the obtained inclinations. The magnetic field in these two coronal holes were more horizontal than this dipole field by $12.9^{\circ}$ on average. The lower the latitude is, the larger is the deviation from the dipole field.

Moreover, we find that EUV plumes and EUV surface bright points are not always related, which is consistent with the observations of @Wang:1998 and @Raouafi:etal:2008. Of the three plumes in front of the solar limb on April 7, only one was definitely associated with a bright point. For the other two we did not find a related bright point. Conversely, we saw a bright point in the images to which no plume pair could be assigned to in the two EUVI images. A possible explanation could be that the lifetime of a bright point is shorter than 