  We present measurements of elemental abundances in solar flares with the EUV
Variability Experiment (EVE) on the Solar Dynamics Observatory (SDO). EVE
observes both high temperature Fe emission lines (Fe XV-Fe XXIV) and continuum
emission from thermal bremsstrahlung that is proportional to the abundance of
H. By comparing the relative intensities of line and continuum emission it is
possible to determine the enrichment of the flare plasma relative to the
composition of the photosphere. This is the first ionization potential or FIP
bias ($f$). Since thermal bremsstrahlung at EUV wavelengths is relatively
insensitive to the electron temperature, it is important to account for the
distribution of electron temperatures in the emitting plasma. We accomplish
this by using the observed spectra to infer the differential emission measure
distribution and FIP bias simultaneously. In each of the 21 flares that we
analyze we find that the observed composition is close to photospheric. The
mean FIP bias in our sample is $f=1.27\pm0.23$. This analysis suggests that the
bulk of the plasma evaporated during a flare comes from deep in the
chromosphere, below the region where elemental fractionation occurs.
