exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes

exoALMA. VII. Benchmarking Hydrodynamics and Radiative Transfer Codes

Forward modeling is often used to interpret substructures observed in protoplanetary disks. To ensure the robustness and consistency of the current forward-modeling approach from the community, we conducted a systematic comparison of various hydrodynamics and radiative transfer codes. Using four gri...

Full description

Saved in:
Bibliographic Details
Main Authors: Jaehan Bae, Mario Flock, Andrés Izquierdo, Kazuhiro Kanagawa, Tomohiro Ono, Christophe Pinte, Daniel J. Price, Giovanni P. Rosotti, Gaylor Wafflard-Fernandez, Geoffroy Lesur, ‪Frédéric Masset, Sean M. Andrews, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Stefano Facchini, Daniele Fasano, Maria Galloway-Sprietsma, Cassandra Hall, Iain Hammond, Jane Huang, Giuseppe Lodato, Cristiano Longarini, Jochen Stadler, Richard Teague, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Format: Article
Language:English
Published: IOP Publishing 2025-01-01
Series:The Astrophysical Journal Letters
Subjects:
Protoplanetary disks
Planetary-disk interactions
Hydrodynamical simulations
Radiative transfer simulations
Online Access:https://doi.org/10.3847/2041-8213/adc436
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:Forward modeling is often used to interpret substructures observed in protoplanetary disks. To ensure the robustness and consistency of the current forward-modeling approach from the community, we conducted a systematic comparison of various hydrodynamics and radiative transfer codes. Using four grid-based hydrodynamics codes ( FARGO3D , Idefix , Athena++ , and PLUTO ) and a smoothed-particle hydrodynamics code ( Phantom ), we simulated a protoplanetary disk with an embedded giant planet. We then used two radiative transfer codes ( mcfost and RADMC-3D ) to calculate disk temperatures and create synthetic ^12 CO cubes. Finally, we retrieved the location of the planet from the synthetic cubes using DISCMINER . We found strong consistency between the hydrodynamics codes, particularly in the density and velocity perturbations associated with planet-driven spirals. We also found a good agreement between the two radiative transfer codes: the disk temperature in mcfost and RADMC-3D models agrees within ≲3% everywhere in the domain. In synthetic ^12 CO channel maps, this results in brightness temperature differences within ±1.5 K in all our models. This good agreement ensures consistent retrieval of planet’s radial/azimuthal location with only a few percent of scatter, with velocity perturbations varying ≲20% among the models. Notably, while the planet-opened gap is shallower in the Phantom simulation, we found that this does not impact the planet location retrieval. In summary, our results demonstrate that any combination of the tested hydrodynamics and radiative transfer codes can be used to reliably model and interpret planet-driven kinematic perturbations.
ISSN:2041-8205

Similar Items