Elemental abundances in the solar corona, plotted against the First
Ionization Potential (FIP) of each element, from UVCS and SUMER data
(see Raymond et al. 1997, Solar Physics, 175, 645; and Feldman et al.
1998, ApJ, 505, 999).  The UVCS data were obtained at 1.5 solar radii
and the SUMER data pertain to heights below 1.03 solar radii.  Each
elemental abundance is divided by the photospheric abundance and
plotted on a logarithmic scale.  For comparison with the three sets
of observational data, the dotted lines show a FIP bias of 4 matched
to the high-FIP elements (i.e., with FIP above about 10 eV) for
each data set.