Abstract: Since the development of planetary science, more than 5000 exoplanets have been discovered. Understanding the evolution of protoplanetary disks is essential to clarify the classification of exoplanets and improve the efficiency of exoplanet detection. At the same time, exoplanet observations can be used to constrain and examine the physical parameters of the interaction between the protoplanetary disk and the planet. Therefore, in this paper, the surface density of the protoplanetary disk is linked to the star mass, combined with the distribution of exoplanet properties, and the interaction process between planets with different masses and specific protoplanetary disks is simulated by using the fluid dynamics code FARGO3D. Simulation results show that: (1) there is a power-law relationship between the relative surface density of the gap structure and the mass of the planet, and the power-law exponent has a strong correlation with the mass of the star; (2) there is a power-law relationship between the duration of the gap structure and the mass of the planet, and the power-law exponent has a weak correlation with the mass of the star; (3) there is a log-linear relationship between the width of the gap structure and the mass of the planet, and the power-law exponent has a weak correlation with the mass of the star. That is, the strength of the interaction between the planet and the protoplanetary disk is not only reflected in the relative surface density of the gap structure in the stable state, but also in the duration and width of the gap structure.