  We find that the element abundances in solar energetic particles (SEPs) and
in the slow solar wind (SSW), relative to those in the photosphere, show
different patterns as a function of the first ionization potential (FIP) of the
elements. Generally, the SEP and SSW abundances reflect abundance samples of
the solar corona, where low-FIP elements, ionized in the chromosphere, are more
efficiently conveyed upward to the corona than high-FIP elements that are
initially neutral atoms. Abundances of the elements, especially C, P, and S
show a crossover from low to high FIP at ~10 eV in the SEPs but ~14 eV for the
solar wind. Naively this seems to suggest cooler plasma from sunspots beneath
active regions. More likely, if the ponderomotive force of Alfv\'en waves
preferentially conveys low-FIP ions into the corona, the source plasma that
eventually will be shock-accelerated as SEPs originates in magnetic structures
where Alfv\'en waves resonate with the loop length on closed magnetic field
lines. This concentrates FIP fractionation near the top of the chromosphere.
Meanwhile, the source of the SSW may lie near the base of diverging open-field
lines surrounding, but outside of, active regions, where such resonance does
not exist, allowing fractionation throughout the chromosphere. We also find
that energetic particles accelerated from the solar wind itself by shock waves
at corotating interaction regions (CIRs), generally beyond 1 AU, confirm the
FIP pattern of the solar wind.
