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Mapping lithium evolution for evolved stars will provide restrictions andconstraints on the fundamental stellar interior physical processes, whichfurther shed light on our understanding of the theory of stellar structure andevolution. Based on a sample of 1,848 giants with known evolutionary phases andlithium abundances from the LAMOST-\kepler{} and LAMOST-\emph{K}2 fields, weconstruct mass-radius diagrams to characterize the evolutionary features oflithium. The stars at red giant branch (RGB) phase show natural depletion alongwith their stellar evolution, particularly, there is no obvious crowd starswith anomalously high Li abundances near the bump. Most of the low-mass starsreaching their zero-age sequence of core-helium-burning (ZAHeB) have Liabundances around $\sim1.0$\,dex, which show an increase of Li abundance by$\sim0.6$\,dex compared to the stars above the bump of RGB. This suggests thehelium flash can be responsible for moderate Li production. While for superLi-rich stars, some special mechanisms should be considered during heliumflash. Other scenarios, such as merger, could also be interpretations given theLi-rich stars can be found at anytime during the steady state phase of coreHe-burning. During the core He-burning (HeB) phase, there is no indication ofobvious lithium depletion.

Lithium Evolution of Giant Stars Observed by LAMOST and Kepler