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Coronal plumes, which extend from solar coronal holes (CH) into the highcorona and - possibly - into the solar wind (SW), can now continuously bestudied with modern telescopes and spectrometers on spacecraft, in addition toinvestigations from the ground, in particular, during total eclipses. Despitethe large amount of data available on these prominent features and relatedphenomena, many questions remained unanswered as to their generation andrelative contributions to the high-speed streams emanating from CHs. Anunderstanding of the processes of plume formation and evolution requires abetter knowledge of the physical conditions at the base of CHs, in plumes andin the surrounding inter-plume regions (IPR). More specifically, information isneeded on the magnetic field configuration, the electron densities andtemperatures, effective ion temperatures, non-thermal motions, plumecross-sections relative to the size of a CH, the plasma bulk speeds, as well asany plume signatures in the SW. In spring 2007, the authors proposed a study on"Structure and dynamics of coronal plumes and inter-plume regions in solarcoronal holes" to the International Space Science Institute (ISSI) in Bern toclarify some of these aspects by considering relevant observations and theextensive literature. This review summarizes the results and conclusions of thestudy. Stereoscopic observations allowed us to include three-dimensionalreconstructions of plumes. Multi-instrument investigations carried out duringseveral campaigns led to progress in some areas, such as plasma densities,temperatures, plume structure and the relation to other solar phenomena, butnot all questions could be answered concerning the details of plume generationprocess(es) and interaction with the SW.

Morphology, dynamics and plasma parameters of plumes and inter-plume regions in solar coronal holes