Modeling of Protoplanetary Disks Based on Radmc-3D

Abstract

From the early stages of star formation to the formation of planetary systems, stars are surrounded by a disk of material that changes in structure and properties as the stars and planets evolve. This disk of material is called the protoplanetary disk, which consists of a large amount of dust and gas, and with the formation of planetary systems, the protoplanetary disk further evolves into a debris disk. The structure of the protoplanetary disk is closely related to the growth of the planets in the disk, and its diversity contributes to the diversity of planetary systems, so the study of protoplanetary disks is of great significance to the understanding of planetary formation and evolution. In this paper, we introduce the evolution of protoplanetary disks and the theoretical methods needed to construct their models. The simulation process of protoplanetary disks is understood by applying the RADMC-3D software package. In addition, I we collected the physical parameters of HL Tauri from the literature, applied these parameters to RADMC-3D for simulation, and analyzed the results of the simulation. Meanwhile, this paper also introduces the important role of the new generation of radio interferometric arrays in the field of protoplanetary disk observation.