Figure 1: EIS images of the solar corona. | Nature Communications

Figure 1: EIS images of the solar corona.

From: Full-Sun observations for identifying the source of the slow solar wind

Figure 1

These pure temperature images are constructed from EIS spectral line intensities and cover a range of temperatures from 0.45 to 2.8 MK. They are used to construct EM distributions at every pixel. The mosaic is constructed by recording the top and bottom readings of the EIS CCD at 26 positions on the solar disk. The observing sequence scans across the central disk, around the North limb and finally around the South limb. It is sheared East-West in some locations because of solar rotation during the 2-day spectrometer scan. Details of the observing sequence are given in the main text.

Back to article page