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Context. The advent of multi-dimensional solar flare simulations has led tonumerous investigations of coronal flows and new physical insights. Thesestudies have not yet included detailed analysis of the lower atmosphericresponses such as down-flowing chromospheric compressions and chromosphericevaporation processes.  Aims. In this work, we present an analysis of multi-dimensional flaresimulations, including analysis of chromospheric up-flows and down-flows thathelp to elucidate multi-dimensional effects. We also provide importantgroundwork for comparing 1D and multi-dimensional models, with the aim thatfuture multi-dimensional simulations can include detailed field-alignedphysical processes.  Methods. A localized anomalous resistivity initiates magnetic reconnection,which drives the evolution of a standard solar flare model. We vary thebackground magnetic field strength, to produce four flare simulations thatcover a large span of observationally reported solar flare strengths.Chromospheric energy fluxes, and energy density maps are used to analyse thetransport of energy from the corona to the lower atmosphere, and the resultantevolution of the flare. Quantities traced along 1D field-lines allow fordetailed comparison with 1D evaporation models. We highlight the similarities,stressing deficiencies from simplified physics along these 1D flux tubes, andcrucial effects that enter by multi-dimensional effects.

Exploring self-consistent 2.5 D flare simulations with MPI-AMRVAC