Masses of W Ursae Majoris-type (W UMa) binaries play a critical role in investigating stellar dynamical evolutionary status. In this paper, we combine the PARSEC (PAdova and TRieste Stellar Evolution Code) with the Roche geometric model to provide a method to determine the masses of W UMa systems. To verify the validity of this method, we compile a sample of 140 spectrum binaries from the literature, which includes 76 W- and 64 A-subtype systems with reliable physical parameters. We find that the average fractional difference and the standard deviation (σM) of the residuals for W-subtype and A-subtype approximately amount to 15.66% and 0.1218, 16.03% and 0.2094, respectively. Meanwhile, we also perform detailed analyses in accordance with the orbital period, the effective temperatures and the mass ratio. We find that the method is more applicable to determine masses for W UMa systems with low effective temperature and short period.

大熊座 W 型 (W UMa) 双星的质量在研究恒星动力学演化状态方面发挥着关键作用。在本文中，我们将 PARSEC（PAdova 和 Trieste 恒星演化代码）与 Roche 几何模型相结合，提供了一种确定 W UMa 系统质量的方法。为了验证该方法的有效性，我们从文献中编译了 140 个光谱二进制文件的样本，其中包括具有可靠物理参数的 76 个 W 和 64 个 A 亚型系统。我们发现平均分数差和标准差 ( σM) W 亚型和 A 亚型的残差分别约为 15.66% 和 0.1218、16.03% 和 0.2094。同时，我们还根据轨道周期、有效温度和质量比进行了详细的分析。我们发现该方法更适用于有效温度低、周期短的 W UMa 系统的质量测定。