  In this study, we explore the evolution of lithium in giant stars based on
data assembled from the literature on asteroseismology and Li abundances for
giants. Our final sample of 187 giants consists of 44 red giant branch (RGB),
140 core He-burning (CHeB) and three giants with an unclassified evolutionary
phase. For all 187 stars, the seismic parameters $\nu\rm_{max}$ (frequency of
maximum oscillation power) and $\Delta \nu$ (large frequency spacing) are
available, while $\Delta \Pi\rm_{1}$ (the asymptotic gravity-mode period
spacing) is available for a subset of 64. For some of the CHeB giants, mass
estimates from the asteroseismic scaling relations are found to be
underestimated when compared with mass estimates from isochrones based on
seismic data. Whilst most of the Li-rich giants in the sample have masses less
than 1.5 $M_\odot$, they are also present up to and beyond the maximum mass
expected to have suffered a core He-flash, i.e. $M$ $\leq$ 2.25 $M_\odot$: this
suggests contributions from other processes towards Li enrichment. To
understand the evolution of giants in the $\Delta \Pi\rm_{1}$ $-$ $\Delta \nu$
plane, we use the {\it Modules for Experiments in Stellar Astrophysics} models
which show the presence of mini He-flashes following the initial strong core
He-flash. From the distribution of A(Li) as a function of $\Delta \nu$, which
is similar to the distribution of A(Li) as a function of luminosity, we find no
indication of Li enrichment near the luminosity bump. Also, A(Li) trends to
$\sim$ -1.5 dex near the RGB tip. The data also suggest a decrease in A(Li)
with an increase in $\Delta \Pi\rm_{1}$ for CHeB giants.
