Fig. 7
Elemental abundances in solar units of the six coronae (black symbols) as a function of the first ionization potential (FIP) compared with the photospheric values (red). Line at 1 represents solar (Asplund et al. 2009). Note photospheric abundance ranges represent literature ranges and not actual uncertainties. A FIP effect is observed for ι Hor, HR 7291, α Cen A and B, which is not true for 11 LMi and τ Boo. Clearly, abundance trends relative to solar and relative to actual photospheric values are not always consistent.
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