The F-CHROMA project aims to answer a number of top-level science questions including:
- What is the energy output of the flaring chromosphere?
- Can we develop a self-consistent quasi-3D model of the flare chromosphere that will reproduce the dominant chromospheric lines and continua?
- Is the standard ‘collisional thick-target’ model for flare energy transport correct, and are there viable alternatives?
- What are the observational signatures of an out-of-equilibrium chromospheric plasma including electron, and possibly proton, distributions?
- How does the temperature, density and ionization structure of the flare chromosphere respond to time-dependent energy input?
- What do our models tell us about the flares that are observed in other solar-type stars?
Our objectives linked to the above questions are to:
- Perform joint observations and analysis of space-based and ground-based observations of flares, delivering improved diagnostics for conditions in the flare chromosphere;
- Carry out detailed modeling of these diagnostics for a range of flare energy inputs
- Utilize forward modeling techniques to determine the physical properties of the solar chromosphere during solar flares;
- Use models and observations to optimize targeted flare observing sequences for present and future missions and observatories, hence maximizing their scientific return;
- Produce a catalogue of existing and future ground-based solar flare observations, linked to available space-based counterparts;
- Populate an archive of ground-based flare observations and make it available to the community;
- Produce a flare spectral model database and make it available to the community.