resolution ($1.6^{\prime\prime}$ per pixel) and larger field of view (out to 1.7 $R_\odot$). For the objectives of the mission and more details about the EUVI telescopes see @Howard:etal:2008 and @Wuelser:etal:2004.

As the solar activity was low in 2007, the appearance of the solar corona over the poles was dominated by extended raylike features, the so-called polar plumes. They are believed to trace out open magnetic field lines and have been intensively analysed in white light, EUV and soft X-rays. Coordinated observations using the *SOHO* spacecraft and the ground-based HAO (High Altitude Observatory) Mk-3 coronagraph of the polar plumes from the photosphere to approximately 15 $R_\odot$ were presented by @DeForest:etal:1997 and out to 30 $R_\odot$ or 45 $R_\odot$ by @DeForest:etal:2001. @Gabriel:etal:2003 [@Gabriel:etal:2005] have suggested that plumes are a substantial contributors to the fast solar wind, whereas @Habbal:1992; @Wang:1994 and @Wilhelm:etal:2000 have a different point of view. They suggest that the interplume regions are the dominant source of the high-speed solar wind. Another debate about plumes is whether they are rooted in an unipolar magnetic field configuration @Newkirk:Harvey:1968 [@DeForest:etal:1997] or are formed by the unipolar magnetic field reconnected with emerging bipolar regions @Wang:Sheeley:1995.

One handicap of all previous studies was the fact 