  In this work, we studied the distribution of lithium abundances in giants as
a function of stellar mass. We used a sample of 1240 giants common among Kepler
photometric and LAMOST medium resolution (R $\approx$ 7500) spectroscopic
survey fields. The asteroseismic $\Delta$P - $\Delta \nu$ diagram is used to
define core He-burning red clump giants and red giant branch stars with inert
He-core. Li abundances have been derived using spectral synthesis for the
entire sample stars. Directly measured values of asteroseismic parameters
$\Delta$P(or $\Delta \Pi_1$) and $\Delta \nu$ are either taken from the
literature or measured in this study. Of the 777 identified red clump giants,
we found 668 low mass ($\leq$ 2~M$_{\odot}$) primary red clump giants and 109
high mass ($>$ 2~M$_{\odot}$) secondary red clump giants. Observed Li
abundances in secondary red clump giants agree with the theoretical model
predictions. The lack of Li-rich giants among secondary red clump giants and
the presence of Li-rich, including super Li-rich giants, among primary red
clump stars reinforces the idea that Helium-flash holds the key for Li
enrichment among low-mass giants. The results will further constrain
theoretical models searching for a physical mechanism for Li enhancement among
low-mass red clump giants. Results also serve as observational evidence that
only giants with mass less than $\approx$ 2~M$_{\odot}$ develop degenerate
He-core and undergo He-flash.
