  Observations demonstrate that the surface abundance of $^7{\rm Li}$ in
low-mass stars changes dramatically between the tip of the red giant branch and
the red clump. This naturally suggests an association with the helium core
flash, which occurs between these two stages. Using stellar evolution models
and a simple, ad hoc mixing prescription, we demonstrate that the $^7{\rm Li}$
enhancement can be explained by a brief chemical mixing event that occurs at
the time of the first, strongest He sub-flash. The amount of $^7{\rm Be}$
already present above the H-burning shell just before the flash, once it mixes
into the cooler envelope and undergoes an electron capture converting it to
$^7{\rm Li}$, is sufficient to explain the observed abundance at the red clump.
We suggest that the excitation of internal gravity waves by the vigorous
turbulent convection during the flash may provide a physical mechanism that can
induce such mixing.
