IRIS: A Generic Three-Dimensional Radiative Transfer Code

TL;DR

IRIS is a versatile 3D radiative transfer code capable of generating synthetic spectra and images, useful for astrophysical diagnostics and laboratory experiments, with ongoing enhancements for non-LTE and scattering effects.

Contribution

The paper introduces IRIS, a new 3D spectral radiative transfer code with a novel solver and interpolation technique, validated through multiple tests, and designed for broad astrophysical and laboratory applications.

Findings

Validated with searchlight beam test

Compared with 1D plane-parallel model

Demonstrated velocity gradient effect handling

Abstract

We present IRIS, a new generic three-dimensional (3D) spectral radiative transfer code that generates synthetic spectra, or images. It can be used as a diagnostic tool for comparison with astrophysical observations or laboratory astrophysics experiments. We have developed a 3D short-characteristic solver that works with a 3D nonuniform Cartesian grid. We have implemented a piecewise cubic, locally monotonic, interpolation technique that dramatically reduces the numerical diffusion effect. The code takes into account the velocity gradient effect resulting in gradual Doppler shifts of photon frequencies and subsequent alterations of spectral line profiles. It can also handle periodic boundary conditions. This first version of the code assumes Local Thermodynamic Equilibrium (LTE) and no scattering. The opacities and source functions are specified by the user. In the near future, the capabilities of IRIS will be extended to allow for non-LTE and scattering modeling. IRIS has been validated through a number of tests. We provide the results for the most relevant ones, in particular a searchlight beam test, a comparison with a 1D plane-parallel model, and a test of the velocity gradient effect. IRIS is a generic code to address a wide variety of astrophysical issues applied to different objects or structures, such as accretion shocks, jets in young stellar objects, stellar atmospheres, exoplanet atmospheres, accretion disks, rotating stellar winds, cosmological structures. It can also be applied to model laboratory astrophysics experiments, such as radiative shocks produced with high power lasers.