SOLARNET Conference: The Many Scales of the Magnetic Sun

One-dimensional (1D) models of solar flares often generate hot upflows from the chromosphere (chromospheric evaporation) due to heating by energetic particle beams (Allred et al. 2005, 2015, Druett et al. 2017, Polito et al. 2023). The beams of particles are injected at the top of the models using distributions consistent with X-ray emission in observations assumed to result from Bremsstrahlung emission from energetic particle beams impacting the ambient plasma. To date, 2D and 3D flare models produce evaporation as a result of thermal conduction and the delivery of kinetic energy to the lower atmosphere from the outflows of reconnection jets (e.g. Ruan et al. 2020). In this study we evaluate and explore the reasons for this difference compare the differences between the findings of 1D and multi-dimensional flare models. We report the first simulation of chromospheric evaporation in a multi-dimensional model caused by beam electrons.