Development of 1-D non-ideal MHD simulation code towards understanding Long-term Evolution of Protoplanetary Disk

TL;DR

This paper presents a 1-D non-ideal MHD simulation code to study the long-term evolution of protoplanetary disks, capturing key physical processes and producing results consistent with observations.

Contribution

The authors developed a novel 1-D MHD simulation code incorporating non-ideal effects for long-term disk evolution studies.

Findings

Disk size and mass at 10^5 years match observations.

Radial profiles align with analytical solutions.

Magnetic braking influences disk evolution.

Abstract

We developed a one-dimensional magnetohydrodynamic (MHD) simulation code to investigate the long-term evolution of protoplanetary disks with low computational cost. In this simulation code, the physical processes necessary for protostellar formation and protoplanetary disk evolution, such as magnetic braking, non-ideal MHD effects, and angular momentum transport due to viscosity, are implemented. Using this simulation code, we performed the simulations of the long-term evolution of protoplanetary disks starting from the molecular cloud. Our simulation results suggest that the disk size and mass are a few tens of au and $\sim 0.01 M_\odot$ at $10^5$ years after protostellar formation. These values were relatively consistent with observations. The disk evolves through magnetic braking, and its radial profiles are consistent with the analytical solutions of previous studies. Our simulation code will be an important tool for studying the long-term evolution of protoplanetary disks.