本文对天体系统的潮汐锁定问题的一种简化模型进行了研究.本文将中心天体设为由固体球状内核以及外层均匀液体组成，将在引力作用下液体产生的形变近似成椭球形，并说明了该近似的合理性.最后，论文参考“常数几何滞后模型”，在近似条件下计算了当中心天体相对平衡位置具有θ的偏角时所受引力相对其中心的力矩，得出了两天体间潮汐摩擦力矩与绕转天体质量的平方以及中心天体平均半径的5次方成正比，与天体间距离的6次方成反比的结论.

This article investigates a simplified model of tidal locking in celestial binary systems. The central body is assumed to consist of a solid spherical core and a uniform liquid outer layer, and the deformation of the central body under gravity is approximated as ellipsoidal. The precision of this approximation is also demonstrated. Finally, the article uses the “constant geometric lag model” to calculate the tidal torque relative to the centroid of the central body when the central body has a deviation angle of θ from its equilibrium position. The conclusion is that the tidal frictional torque between the two celestial bodies is proportional to the square of the revolving body^,s mass, the fifth power of the central body^,s average radius, and inversely proportional to the sixth power of the distance between the two bodies.