Flare Kernels May be Smaller than You Think: Modelling the Radiative Response of Chromospheric Plasma Adjacent to a Solar Flare

TL;DR

This study models how intense radiation from a solar flare affects nearby chromospheric plasma, revealing that flare kernels may appear larger in spectral lines than they truly are, impacting observational interpretations.

Contribution

It introduces a two-dimensional radiative transfer model to analyze the influence of flare radiation on adjacent chromospheric plasma, highlighting effects on spectral line formation and apparent flare kernel sizes.

Findings

Spectral line cores show significant spatial, temporal, and wavelength variations.

Flare radiation can cause apparent increases in the size of flare kernels in spectral observations.

Continuum intensity remains largely unaffected by the radiation field.

Abstract

Numerical models of solar flares typically focus on the behaviour of directly-heated flare models, adopting magnetic field- aligned, plane-parallel methodologies. With high spatial- and spectral-resolution ground-based optical observations of flares, it is essential also to understand the response of the plasma surrounding these strongly heated volumes. We investigate the effects of the extreme radiation field produced by a heated column of flare plasma on an adjacent slab of chromospheric plasma, using a two-dimensional radiative transfer model and considering the time-dependent solution to the atomic level populations and electron density throughout this model. The outgoing spectra of H$\alpha$ and Ca II 854.2 nm synthesised from our slab show significant spatial-, time-, and wavelength-dependent variations (both enhancements and reductions) in the line cores, extending on order 1 Mm into the non-flaring slab due to the incident transverse radiation field from the flaring boundary. This may lead to significant overestimates of the sizes of directly-heated flare kernels, if line-core observations are used. However, the radiation field alone is insufficient to drive any significant changes in continuum intensity, due to the typical photospheric depths at which they forms, so continuum sources will not have an apparent increase in size. We show that the line formation regions near the flaring boundary can be driven upwards in altitude by over 1 Mm despite the primary thermodynamic parameters (other than electron density) being held horizontally uniform. This work shows that in simple models these effects are significant and should be considered further in future flare modelling and interpretation.