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Solar flares are driven by release of the free magnetic energy and itsconversion to other forms of energy -- kinetic, thermal, and nonthermal.Quantification of partitions between these energy components and theirevolution is needed to understand the solar flare phenomenon includingnonthermal particle acceleration, transport, and escape and the thermal plasmaheating and cooling. The challenge of remote sensing diagnostics is that thedata are taken with finite spatial resolution and suffer from line-of-sight(LOS) ambiguity including cases when different flaring loops overlap andproject one over the other. Here we address this challenge by devising adata-constrained evolving 3D model of a multi-loop SOL2014-02-16T064620 solarflare of GOES class C1.5. Specifically, we employed a 3D magnetic modelvalidated earlier for a single time frame and extended it to cover the entireflare evolution. For each time frame we adjusted the distributions of thethermal plasma and nonthermal electrons in the model, such as the observablessynthesized from the model matched the observations. Once the evolving modelhas been validated this way, we computed and investigated the evolving energycomponents and other relevant parameters by integrating over the model volume.This approach removes the LOS ambiguity and permits to disentanglecontributions from the overlapping loops. It reveals new facets of electronacceleration and transport, as well as heating and cooling the flare plasma in3D. We find signatures of substantial direct heating of the flare plasma notassociated with the energy loss of nonthermal electrons.

Data-constrained 3D modeling of a solar flare evolution: acceleration, transport, heating, and energy budget