The radio galaxy 3C 84 is a representative of γ-ray-bright misaligned active galactic nuclei (AGNs) and one of the best laboratories to study the radio properties of the subparsec jet in connection with the γ-ray emission. In order to identify possible radio counterparts of γ-ray emissions in 3C 84, we study the change in structure within the central 1 pc and the light curve of subparsec-sized components C1, C2 and C3. We search for any correlation between changes in the radio components and the γ-ray flares by making use of the Very Long Baseline Interferometry (VLBI) and single-dish data. Throughout the radio monitoring spanning over two GeV γ-ray flares detected by the Fermi Large Area Telescope and the MAGIC Cherenkov Telescope during 2009 April–May and 2010 June–August, the total flux density in the radio band increases on average. This flux increase mostly originates in C3. Although γ-ray flares span the time-scale of days to weeks, no clear correlation with the radio light curve on this time-scale is found. No new prominent components and change in morphology associated with the γ-ray flares are found on VLBI images.