  The possibility of unaccounted for opacity sources in the UV for late-type
stars has often been invoked to explain discrepancies between predicted and
observed flux distributions and spectral line strengths. Such missing
UV-opacity could among other things have a significant impact on abundance
determination for elements whose only relevant spectral features are accessible
in this wavelength region, such as Be. Here, the study by Balachandran & Bell
(1998) is re-visited in the light of a realistic 3D hydrodynamical solar model
atmosphere and the recently significantly downward revised solar O abundance
obtained with the same model atmosphere. The amount of missing UV-opacity, if
any, is quantified by enforcing that the OH A-X electronic lines around 313 nm
produce the same O abundance as the other available diagnostics: OH
vibration-rotation and pure rotation lines in the IR, the forbidden [OI] 630.0
and 636.3 nm lines and high-excitation, permitted OI lines. This additional
opacity is then applied for the synthesis of the BeII line at 313.0nm to derive
a solar photospheric Be abundance in excellent agreement with the meteoritic
value, thus re-enforcing the conclusions of Balachandran & Bell. The about 50%
extra opacity over accounted for opacity sources can be well explained by
recent calculations by the Iron Project for photo-ionization of FeI.
