User Manual Privacy Policy Disclaimer Contact us
  Advanced SearchBrowse




Journal Article

AREPO-RT: Radiation hydrodynamics on a moving mesh


Springel,  Volker
Computational Structure Formation, MPI for Astrophysics, Max Planck Society;

External Ressource
No external resources are shared
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available

Kannan, R., Vogelsberger, M., Marinacci, F., McKinnon, R., Pakmor, R., & Springel, V. (2019). AREPO-RT: Radiation hydrodynamics on a moving mesh. Monthly Notices of the Royal Astronomical Society, 485(1), 117-149. doi:10.1093/mnras/stz287.

Cite as: http://hdl.handle.net/21.11116/0000-0003-AFA0-3
We introduce AREPO-RT, a novel radiation hydrodynamic (RHD) solver for the unstructured moving-mesh code AREPO. Our method solves the moment-based radiative transfer equations using the M1 closure relation. We achieve second-order convergence by using a slopelimited linear spatial extrapolation and a first-order time prediction step to obtain the values of the primitive variables on both sides of the cell interface. A Harten–Lax–van Leer flux function, suitably modified for moving meshes, is then used to solve the Riemann problem at the interface. The implementation is fully conservative and compatible with the individual time-stepping scheme of AREPO. It incorporates atomic hydrogen (H) and helium (He) thermochemistry, which is used to couple the ultraviolet radiation field to the gas. Additionally, infrared (IR) radiation is coupled to the gas under the assumption of local thermodynamic equilibrium between the gas and the dust.We successfully apply our code to a large number of test problems, including applications such as the expansion of HII regions, radiation pressuredriven outflows, and the levitation of optically thick layer of gas by trapped IR radiation. The new implementation is suitable for studying various important astrophysical phenomena, such as the effect of radiative feedback in driving galactic scale outflows, radiation-driven dusty winds in high-redshift quasars, or simulating the reionization history of the Universe in a self-consistent manner.