Radiation hydrodynamics in simulations of the solar atmosphere

Abstract

Nearly all energy generated by fusion in the solar core is ultimately radiated away into space in the solar atmosphere, while the remaining energy is carried away in the form of neutrinos. The exchange of energy between the solar gas and the radiation field is thus an essential ingredient of atmospheric modeling. The equations describing these interactions are known, but their solution is so computationally expensive that they can only be solved in approximate form in multi-dimensional radiation-MHD modeling. In this review, I discuss the most commonly used approximations for energy exchange between gas and radiation in the photosphere, chromosphere, and corona.

Accepted for publication in Living Reviews in Solar Physics

References in corpus (11)

• CHIANTI - an atomic database for emission lines - Paper XV: Version 9, improvements for the X-ray satellite lines
• Extension of the MURaM radiative MHD code for coronal simulations
• On the generation of solar spicules and Alfvénic waves
• Non-equilibrium hydrogen ionization in 2D simulations of the solar atmosphere
• Temporal evolution of multiple evaporating ribbon sources in a solar flare
• Fluid description of multi-component solar partially ionized plasma
• Radiative diagnostics in the solar photosphere and chromosphere
• Radiative transfer in decomposed domains
• Numerical simulations of quiet Sun magnetic fields seeded by Biermann battery
• Formation of the helium EUV resonance lines
• Structure of the solar photosphere studied from the radiation hydrodynamics code ANTARES

Cited by in corpus (19)

• Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections
• The Visible Spectro-Polarimeter of the Daniel K. Inouye Solar Telescope
• A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
• Observational study of chromospheric heating by acoustic waves
• Quiet-Sun hydrogen Lyman-alpha line profile derived from SOHO/SUMER solar-disk observations
• Heating of the solar chromosphere through current dissipation
• Acoustic-gravity wave propagation characteristics in 3D radiation hydrodynamic simulations of the solar atmosphere
• Mg ii h&k spectra of an enhanced network region simulated with the MURaM-ChE code. Results using 1.5D synthesis
• Small-scale solar jet formation and their associated waves and instabilities
• Spatially resolved spectroscopy across stellar surfaces. IV. F, G, & K-stars: Synthetic 3D spectra at hyper-high resolution
• Irradiance Variations of the Sun and Sun-Like Stars -- Overview of Topical Collection
• Numerical simulations of macrospicule jets under energy imbalance conditions in the solar atmosphere
• IRIS observations of chromospheric heating by acoustic waves in solar quiet and active regions
• Impact of thermal misbalance on acoustic-gravity waves in the solar atmosphere
• Long characteristics vs. short characteristics in 3D radiative transfer simulations of polarized radiation
• Modeling of Chromospheric Features and Dynamics in Solar Plage
• Turbulent radiative diffusion and turbulent Newtonian cooling
• Dark off-limb gap: manifestation of temperature minimum and dynamic nature of the chromosphere
• A single frequency approach to nonequilibrium modeling of the chromosphere