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Analysis of non-thermal velocities in the solar corona

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Figure

Fig. 1. A reconstructed image of the Fe XIV corona made from theseries of observations with the MICA coronagraph in Argentina (seeStenborg et al., 1999)
Fig. 2. Average image of the spectrum taken above the E-limb at adistance of 1.5′ from the limb (this position of the slit is barely seenin Fig
Table 1. Times, positions and numbers of the analysed slit spectra(see Fig. 1).
Table 2. Average for each slit length of the measured parameters of FeXIV line emissions in different locations of the solar corona (seeFig
+2

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