Chandra X-ray observations of Kepler ’ s supernova remnant indicate the existence of a high speed Fe-rich ejecta structure in the southwestern region . We report strong K-shell emission from Fe-peak elements ( Cr , Mn , Fe , Ni ) , as well as Ca , in this Fe-rich structure , implying that those elements could be produced in the inner area of the exploding white dwarf . We found Ca/Fe , Cr/Fe , Mn/Fe and Ni/Fe mass ratios of 1.0–4.1 % , 1.0–4.6 % , 1–11 % and 2–30 % , respectively . In order to constrain the burning regime that could produce this structure , we compared these observed mass ratios with those in 18 one-dimensional Type Ia nucleosynthesis models ( including both near- M _ { Ch } and sub- M _ { Ch } explosion models ) . The observed mass ratios agree well with those around the middle layer of incomplete Si-burning in Type Ia nucleosynthesis models with a peak temperature of \sim ( 5.0–5.3 ) \times 10 ^ { 9 } K and a high metallicity , Z > 0.0225 . Based on our results , we infer the necessity for some mechanism to produce protruding Fe-rich clumps dominated by incomplete Si-burning products during the explosion . We also discuss the future perspectives of X-ray observations of Fe-rich structures in other Type Ia supernova remnants .