Abstract

Modern simulations of isolated structures such as solar prominences and filaments demonstrate increasingly complex and realistic behaviour down to fine spatial scales. However, the lack of self-consistent optically thick radiation treatment limits their comparison to observations. This is primarily due to the difficulty converting magnetohydrodynamic (MHD) simulation cubes into emergent spectra for spectral lines that form outside of local thermodynamic equilibrium (LTE). Whilst complex, these spectral lines are the primary vector by which these structures can be interpreted and are key to exploiting cutting edge solar observatories.

In this talk I will discuss the formation of spectral lines outside of LTE (non-LTE), and the application of these techniques to models of isolated solar structures. I will also touch on potential pitfalls of a column-by-column approach to synthesis and discuss a new approach for scaling to three-dimensional integrated radiative MHD simulations for these structures.