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

TL;DR

This paper presents multi-dimensional solar flare simulations using MPI-AMRVAC, analyzing chromospheric responses like up-flows and down-flows, and compares these with 1D models to improve understanding of flare dynamics.

Contribution

It introduces detailed multi-dimensional flare simulations with energy transport analysis, bridging the gap between 1D and multi-dimensional models.

Findings

Chromospheric energy fluxes vary with magnetic field strength.

Simulations reveal complex chromospheric flow patterns.

Comparison with 1D models shows both similarities and differences.

Abstract

Context. Multi-dimensional solar flare simulations have not yet included detailed analysis of the lower atmospheric responses such as down-flowing chromospheric compressions and chromospheric evaporation processes. Aims. We present an analysis of multi-dimensional flare simulations, including analysis of chromospheric up-flows and down-flows that provide important groundwork for comparing 1D and multi-dimensional models. Methods. We follow the evolution of an MHD standard solar flare model including electron beams, where localized anomalous resistivity initiates magnetic reconnection. We vary the background magnetic field strength, to produce simulations that cover a large span of observationally reported solar flare strengths. Chromospheric energy fluxes, and energy density maps are used to analyse the transport of energy from the corona to the lower atmosphere, and the resultant evolution of the flare. Quantities traced along 1D field-lines allow for detailed comparison with 1D evaporation models.