Main Objective: Measure Doppler velocities, temperatures, densities, and abundances in a polar coronal hole, Quiet Sun, and their boundary to be compared with the densities, temperatures, and speeds in the extended solar corona seen in coronagraphic images.
Scientific justification: The solar atmosphere is highly structured due to the complexity of coronal magnetic fields. Such complex structures result in differences in temperature and speed of the solar wind. To understand the physical processes of the coronal heating and solar wind acceleration, we investigate the physical characteristics of various chromosphere, transition region, and coronal structures. This includes (1) the footpoints of plumes and inter-plumes in a polar coronal hole, (2) Quiet Sun adjacent to the coronal hole where the plumes originate from. (3) Coronal bright points in the coronal hole on solar disk. Hinode/EIS data will be employed to determines the mass of outflows, temperature, and abundances, as well as the properties of waves and shocks. EUV and coronagraphic images will be used to investigate the response of the upper atmosphere of these coronal base features. To pinpoint such specific regions listed above, we will use the most recent EUV images taken from SDO/AIA and STEREO/EUVI, as well as coronagraphic images obtained from SOHO/LASCO C2/C3 and STEREO/COR1/COR2.
This coordinated observation consists of BBSO (Big Bear Solar Observatory) GST (Goode Solar Telescope), IRIS, and Hinode/EIS. BBSO/GST and IRIS will probe the chromospheric outflows associated with structures observed in coronagraphic images (polar plumes, inter-plumes, and streamers). Hinode/EIS will fill up the gap between the outflows and the solar wind properties.
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