Development of a one-dimensional simulation code for the long-term evolution of protoplanetary disks

Yudai Kobayashi, Daisuke Takaishi, Yusuke Tsukamoto

Recent improvements in observational techniques have made it possible to observe the detailed structure of protoplanetary disks. For instance, ring and gap structures have been discovered in disks around Class II objects by ALMA telescope observations. These structures are considered evidence of planet formation and are crucial for investigating when and how planets form.

On the other hand, according to theory, magnetic fields play a crucial role in the formation and evolution of protoplanetary disks. It has been investigated, mainly using 3D magnetohydrodynamics (MHD) simulations [Machida et al.(2011); Tomida et al. (2015); Masson et al.(2016); Tsukamoto et al.(2017); Wurster and Bate 2019].

However, 3D simulations are difficult to investigate the long-term evolution of protoplanetary disks because of their enormous computational cost. It is a crucial issue that even the newest supercomputer can not resolve. Furthermore, the recent observation requires the simulation of disk evolution in realistic magnetic fields about a million years after protostar formation. Therefore, in this study, we develop a 1D simulation code with light computational cost and reveal the long-term evolution of protoplanetary disks over about a million years, from the gravitational contraction of molecular cloud cores to Class II objects. In this poster, we discuss the result of about half a million years from the gravitational contraction of the molecular cloud core.