The elemental abundance in the solar corona is different from the photosphere. The fractionation between photospheric and coronal abundances is related to the “First Ionization Potential (FIP) effect.” In the corona, the low FIP (FIP < 10 eV) elements are enhanced by factors of 3–4 relative to the photospheric abundances. In contrast, the high FIP elemental abundance ratio to photospheric is approximately equal. Still, it is not revealed how the solar abundance is fractionated. Recently, the most probable model is “Abundance fractionation by the Pondermotive force”. The pondermotive force induced by the Alfvén wave preferentially affects the ionized elements (low FIP element), not the neutral in the chromospheric plasma, which is partially ionized. Then, the force drags up (or down) the low FIP elements depending on the Alfvén wave existence and their energy density in the chromosphere. For investigating the relations between the abundance fractionation and wave energy density in the chromosphere, we analyze the H alpha and Ca II data from GST/FISS for the Alfvén wave detection and Si X (low FIP element) and S X (high FIP element) spectra from Hinode/EIS for determining the relative abundance in an active region. We present the result of detecting Alfvén waves in the chromosphere compared to the spatial distribution of the abundance fractionation.