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Context: Stars with about 1$-$2 solar masses at the red giant branch (RGB)represent an intriguing period of stellar evolution, i.e. when the convectiveenvelope interacts with the fast-rotating core. During these mixing episodesfreshly synthesized lithium can come up to the stellar surface along with highangular momentum material. This high angular momentum may alter the surfacerotation pattern.  Aims: The single rapidly rotating K-giant V1192 Ori is revisited to determineits surface differential rotation, lithium abundance, and basic stellarproperties such as a precise rotation period. The aim is to independentlyverify the antisolar differential rotation of the star and possibly find aconnection to the surface lithium abundance.  Methods: We applied time-series Doppler imaging to a new multi-epoch dataset. Altogether we reconstructed 11 Doppler images from spectroscopic datacollected with the STELLA robotic telescope between 2007--2016. We used ourinversion code iMap to reconstruct all stellar surface maps. We extracted thedifferential rotation from these images by tracing systematic spot migration asa function of stellar latitude from consecutive image cross-correlations.  Results: The position of V1192 Ori in the Hertzsprung-Russell diagramsuggests that the star is in the helium core-burning phase just leaving the RGBbump. We measure $A({\rm Li})_{\rm NLTE}=1.27$, i.e. a value close to theanticipated transition value of 1.5 from Li-normal to Li-rich giants. Dopplerimages reveal extended dark areas arranged quasi-evenly along an equatorialbelt. No cool polar spot is found during the investigated epoch. Spotdisplacements clearly suggest antisolar surface differential rotation with$\alpha=-0.11\pm0.02$ shear coefficient.  Conclusions: The surface Li enrichment and the peculiar surface rotationpattern may indicate a common origin.

Antisolar differential rotation with surface lithium enrichment on the single K-giant V1192 Orionis