Raouafi & Stenborg (2014, ApJ, 787, 118) recently found that coronal hole plumes demonstrate a large number of small jets (termed jetlets) and transient bright points that are due to the quasi-random cancellation of magnetic fragments at the plume footpoints, and suggested that these are the main energy source for plumes.
In this IHOP we will extend this analysis using the high spatial resolution of SOT to resolve the small-scale magnetic field at the plume bases, and use IRIS to search for evidence of reconnection through Doppler shifts and broadening of transition region and chromosphere lines. In addition, coronal emission lines of EIS will be used to search for transient brightenings and line broadening in the corona that result from the energy release.
Target ------ A plume should be identified in either a low-latitude extension to a coronal hole, or an equatorial coronal hole. The combined 171-193-211 images available at http://sdowww.lmsal.com/suntoday are recommended for identifying plumes in coronal holes as they show up as blue features within dark coronal holes.
Duration -------- A duration of 4 hours is requested in order to monitor the evolution of the plume. |
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