Simulation of Thermal Surface Waves in a Protoplanetary Disk in a Two-Dimensional Approximation

Abstract

Theoretical models predict that the obscuration of stellar radiation by irregularities on the surface of a protoplanetary disk can cause self-generating waves traveling towards the star. However, this process is traditionally simulated using the 1+1D approach, the key approximations of which - vertical hydrostatic equilibrium of the disk and vertical diffusion of IR radiation - can distort the picture. This article presents a two-dimensional radiative hydrodynamic model of the evolution of an axially symmetric gas and dust disk. Within this model, but using simplified assumptions from 1+1D models, we have reproduced the spontaneous generation and propagation of thermal surface waves. The key conclusion of our work is that taking into account two-dimensional hydrodynamics and diffusion of IR radiation suppresses the spontaneous generation and development of thermal waves observed in the 1+1D approximation. The search for the possibility of the existence of surface thermal waves should be continued by studying the problem for various parameters of protoplanetary disks.

arXiv commentAccepted for publication in Astronomy Reports (2022)

References in corpus (11)

• Streaming Instabilities in Protoplanetary Disks
• Rosseland and Planck Mean Opacities for Protoplanetary Discs
• Linear and nonlinear evolution of the vertical shear instability in accretion discs
• Convective Overstability in radially stratified accretion disks under thermal relaxation
• On the survival of zombie vortices in protoplanetary discs
• Thermal Waves in Irradiated Protoplanetary Disks
• Thermal Wave Instability as an Origin of Gap and Ring Structures in Protoplanetary Disks
• Improving the thin-disk models of circumstellar disk evolution. The 2+1-dimensional model
• Evolution of a Viscous Protoplanetary Disk with Convectively Unstable Regions
• Simulations of thermal surface waves in a protoplanetary disk using 1+1D approximation
• Explosive instability of dust settling in a protoplanetary disc

Cited by in corpus (3)

• Radiative Nonideal MHD Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
• Time-dependent response of protoplanetary disk temperature to an FU Ori-type luminosity outburst
• Starlight-driven flared-staircase geometry in radiation hydrodynamic models of protoplanetary disks