Radiative transfer in very optically thick circumstellar disks

TL;DR

This paper introduces two efficient diffusion approximation methods for Monte Carlo radiative transfer simulations in optically thick circumstellar disks, improving accuracy and reducing computation time, and implements them in the MCMax code.

Contribution

The paper presents novel diffusion approximation techniques integrated into MCMax, enhancing simulation speed and accuracy for modeling dense circumstellar disks.

Findings

Diffusion approximations improve temperature structure accuracy.

Methods reduce computation time significantly.

Enhanced modeling of vertical disk structure.

Abstract

In this paper we present two efficient implementations of the diffusion approximation to be employed in Monte Carlo computations of radiative transfer in dusty media of massive circumstellar disks. The aim is to improve the accuracy of the computed temperature structure and to decrease the computation time. The accuracy, efficiency and applicability of the methods in various corners of parameter space are investigated. The effects of using these methods on the vertical structure of the circumstellar disk as obtained from hydrostatic equilibrium computations are also addressed. Two methods are presented. First, an energy diffusion approximation is used to improve the accuracy of the temperature structure in highly obscured regions of the disk, where photon counts are low. Second, a modified random walk approximation is employed to decrease the computation time. This modified random walk ensures that the photons that end up in the high-density regions can quickly escape to the lower density regions, while the energy deposited by these photons in the disk is still computed accurately. A new radiative transfer code, MCMax, is presented in which both these diffusion approximations are implemented. These can be used simultaneously to increase both computational speed and decrease statistical noise. We conclude that the diffusion approximations allow for fast and accurate computations of the temperature structure, vertical disk structure and observables of very optically thick circumstellar disks.