FUors are believed in the outburst phase of the episodic accretion model with accretion mass rates enhanced by 2-3 orders of magnitude compared to the normal classical T-Tauri stars. We have been monitoring HBC 722, which was brightened by ~5 mag in the V band in 2010 and thus became a new FUor, with BOES. We also observed two other FUors, FU Ori and V1057 Cyg with BOES. V1057 Cyg has been monitored in the optical spectroscopy for decades since its outburst. We present the results of our 2-year monitoring observations of HBC 722 in comparison with FU Ori and V1057 Cyg.