Figure 4: EIS Doppler velocity map of the corona at 2 MK.
From: Full-Sun observations for identifying the source of the slow solar wind
Full-Sun coronal Doppler velocity map derived from single Gaussian fits to the Fe XIII 202.044 Å spectral line. Blue areas highlight plasma that is flowing towards the observer. Red areas highlight plasma that is flowing away from the observer. Vertical artefacts result from the thermal orbital variation of the spectra and should be ignored. The image is scaled to within ±15 km s−1. We discuss the details of the velocity derivation method in the main text.
