Fast and accurate frequency-dependent radiation transport for hydrodynamics simulations in massive star formation

TL;DR

This paper presents a new three-dimensional frequency-dependent radiation transport algorithm that combines speed and accuracy, enabling efficient and precise hydrodynamics simulations of massive star formation.

Contribution

The authors introduce a novel radiation transport method that merges Flux Limited Diffusion with ray-tracing, improving simulation speed and accuracy in modeling massive star formation environments.

Findings

The scheme accurately reproduces temperature distributions in various optical depth regimes.

It matches results from full Monte-Carlo radiative transfer codes.

The method scales well with parallel computing, suitable for complex simulations.

Abstract

Context: Radiative feedback plays a crucial role in the formation of massive stars. The implementation of a fast and accurate description of the proceeding thermodynamics in pre-stellar cores and evolving accretion disks is therefore a main effort in current hydrodynamics simulations. Aims: We introduce our newly implemented three-dimensional frequency dependent radiation transport algorithm for hydrodynamics simulations of spatial configurations with a dominant central source. Methods: The module combines the advantage of the speed of an approximate Flux Limited Diffusion (FLD) solver with the high accuracy of a frequency dependent first order ray-tracing routine. Results: We prove the viability of the scheme in a standard radiation benchmark test compared to a full frequency dependent Monte-Carlo based radiative transfer code. The setup includes a central star, a circumstellar flared disk, as well as an envelope. The test is performed for different optical depths. Considering the frequency dependence of the stellar irradiation, the temperature distributions can be described precisely in the optically thin, thick, and irradiated transition regions. Resulting radiative forces onto dust grains are reproduced with high accuracy. The achievable parallel speedup of the method imposes no restriction on further radiative (magneto-) hydrodynamics simulations. Conclusions: The proposed approximate radiation transport method enables frequency dependent radiation hydrodynamics studies of the evolution of pre-stellar cores and circumstellar accretion disks around an evolving massive star in a highly efficient and accurate manner.