We present the first detailed abundance analysis of the metal-poor giant HKII 17435À00532. This star was observed as part of the University of Texas long-term project Chemical Abundances of Stars in the Halo (CASH). A spectrum was obtained with the High Resolution Spectrograph (HRS) on the Hobby-Eberly Telescope with a resolving power of R $ 15;000. Our analysis reveals that this star may be located on the red giant branch, red horizontal branch, or early asymptotic giant branch. We find that this metal-poor (½Fe/H ¼ À2:2) star has an unusually high lithium abundance [log "(Li) ¼ þ2:1], mild carbon (½C/Fe ¼ þ0:7) and sodium (½Na /Fe ¼ þ0:6) enhancement, as well as enhancement of both s-process (½Ba /Fe ¼ þ0:8) and r-process (½Eu / Fe ¼ þ0:5) material. The high Li abundance can be explained by self-enrichment through extra mixing that connects the convective envelope with the outer regions of the H-burning shell. If so, HKII 17435À00532 is the most metal-poor star in which this short-lived phase of Li enrichment has been observed. The Na and n-capture enrichment can be explained by mass transfer from a companion that passed through the thermally pulsing AGB phase of evolution with only a small initial enrichment of r-process material present in the birth cloud. Despite the current nondetection of radial velocity variations (over $180 days), it is possible that HKII 17435À00532 is in a long-period or highly inclined binary system, similar to other stars with similar n-capture enrichment patterns.