  In this study, we investigated the energy partition of four confined
circular-ribbon flares (CRFs) near the solar disk center, which are observed
simultaneously by SDO, GOES, and RHESSI. We calculated different energy
components, including the radiative outputs in 1$-$8, 1$-$70, and 70$-$370
{\AA}, total radiative loss, peak thermal energy derived from GOES and RHESSI,
nonthermal energy in flare-accelerated electrons, and magnetic free energy
before flares. It is found that the energy components increase systematically
with the flare class, indicating that more energies are involved in larger
flares. The magnetic free energies are larger than the nonthermal energies and
radiative outputs of flares, which is consistent with the magnetic nature of
flares. The ratio $\frac{E_{nth}}{E_{mag}}$ of the four flares, being
0.70$-$0.76, is considerably higher than that of eruptive flares. Hence, this
ratio may serve as an important factor that discriminates confined and eruptive
flares. The nonthermal energies are sufficient to provide the heating
requirements including the peak thermal energy and radiative loss. Our findings
impose constraint on theoretical models of confined CRFs and have potential
implication for the space weather forecast.
