The F-CHROMA grid of 1D RADYN flare models

Abstract

Context: Solar flares are the result of the sudden release of magnetic energy in the corona. Much of this energy goes into accelerating charged particles to high velocity. These particles travel along the magnetic field and the energy is dissipated when the density gets high enough, primarily in the solar chromosphere. Modelling this region is difficult because the radiation energy balance is dominated by strong, optically thick spectral lines. Aims: Our aim is to provide the community with realistic simulations of a flaring loop with an emphasis on the detailed treatment of the chromospheric energy balance. This will enable a detailed comparison of existing and upcoming observations with synthetic observables from the simulations, thereby elucidating the complex interactions in a flaring chromosphere. Methods: We used the 1D radiation hydrodynamics code RADYN to perform simulations of the effect of a beam of electrons injected at the apex of a solar coronal loop. A grid of models was produced, varying the total energy input, the steepness, and low-energy cutoff of the beam energy spectrum. Results: The full simulation results for a grid of models are made available online. Some general properties of the simulations are discussed.

11 pages, 9 figures. Accepted for publication in Astronomy & Astrophysics

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• Flare heating of the chromosphere: Observations of flare continuum from GREGOR and IRIS
• A Seven-Day Multi-Wavelength Flare Campaign on AU Mic III: Quiescent and Flaring Properties of the X-ray Spectra and Chromospheric lines
• Predicted white-light solar flare emission from the F-CHROMA grid of models
• Young M dwarfs flare activity model: Towards better exoplanetary atmospheric characterisation
• Small-Scale and Transient EUV Kernels in Solar Flare Ribbons
• Statistical Study of Balmer Continuum Enhancement in Solar Flares