The magnetic field of ultraluminous X-ray (ULX) pulsars is the key parameter to understand the nature and accretion physics. However, the typical magnetic field values in these ULX pulsars are still under debate. We used six different torque models to study the magnetic fields of ULX pulsars, to see how derived magnetic fields change with different models, and to determine which models are more suitable for ULX pulsars. We took the currently available period, period derivative, and flux data of 7 confirmed ULX pulsars, M82 X-2, ULX NGC 7793 P13, ULX NGC 5907, NGC 300 ULX1, NGC 1313 X-2, M51 ULX-7, Swift J0243.6+6124, plus one potential ULX pulsars, SMC X-3. The magnetic fields of these ULX pulsars were constrained from two physical conditions: the spin-up process and near equilibrium. We checked possible dependence of the magnetic field estimations on the different torque models. The calculations suggest the accretion torque models by Ghosh and Lamb (1979), Wang (1995), Kluźniak and Rappaport (2007) and Campbell (2012) are more likely to support magnetar models for ULX pulsars, while Lovelace et al. (1995)'s model generally predicts the magnetic field in normal neutron stars. Implications of our results combined with other independent methods are also discussed, which will help us to understand the nature and rotational behavior of these ULX pulsars.

超亮 X 射线 (ULX) 脉冲星的磁场是了解自然和吸积物理的关键参数。然而，这些 ULX 脉冲星的典型磁场值仍在争论中。我们使用了六种不同的扭矩模型来研究 ULX 脉冲星的磁场，以了解派生磁场如何随不同模型而变化，并确定哪些模型更适合 ULX 脉冲星。我们获取了 7 颗已确认的 ULX 脉冲星、M82 X-2、ULX NGC 7793 P13、ULX NGC 5907、NGC 300 ULX1、NGC 1313 X-2、M51 ULX-7、Swift J0243 的当前可用周期、周期导数和通量数据.6+6124，加上一颗潜在的 ULX 脉冲星，SMC X-3。这些 ULX 脉冲星的磁场受到两个物理条件的限制：自旋过程和接近平衡。我们检查了磁场估计对不同扭矩模型的可能依赖性。计算表明 Ghosh 和 Lamb（1979）、Wang（1995）、Kluźniak 和 Rappaport（2007）以及 Campbell（2012）的吸积扭矩模型更有可能支持 ULX 脉冲星的磁星模型，而 Lovelace 等人 (1995) 的模型通常预测正常中子星的磁场。还讨论了我们的结果与其他独立方法相结合的含义，这将有助于我们了解这些 ULX 脉冲星的性质和旋转行为。s 模型通常预测正常中子星中的磁场。还讨论了我们的结果与其他独立方法相结合的含义，这将有助于我们了解这些 ULX 脉冲星的性质和旋转行为。s 模型通常预测正常中子星中的磁场。还讨论了我们的结果与其他独立方法相结合的含义，这将有助于我们了解这些 ULX 脉冲星的性质和旋转行为。