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The reconstruction of the solar spectral irradiance (SSI) on various timescales is essential for the understanding of the Earth's climate response tothe SSI variability. The driver of the SSI variability is understood to be theintensity contrast of magnetic features present on the Sun with respect to thelargely non-magnetic quiet Sun. However, different spectral synthesis codeslead to diverging projections of SSI variability. In this study we comparethree different radiative transfer codes and carry out a detailed analysis oftheir performance. We perform the spectral synthesis at the continuumwavelength of 665 nm with the Code for Solar Irradiance (COSI), and theRybicki-Hummer (RH), and Max Planck University of Chicago Radiative MHD (MURaM)codes for three 3D MHD simulations snapshots, a non-magnetic case, and MHDsimulations with 100 G, and 200 G magnetic field strength. We determine theintensity distributions, the intensity differences and ratios for the spectralsynthesis codes. We identify that the largest discrepancies originate in theintergranular lanes where the most field concentration occurs. Overall, theapplied radiative transfer codes give consistent intensity distributions. Also,the intensity variation as a function of magnetic field strength for theparticular 100 G and 200 G snapshots agree within the 2-3% range.

Solar Atmosphere Radiative Transfer Model Comparison based on 3D MHD simulations