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Abstract
Abstract The aim of this study is to generate maps of the hard X-ray emission produced by energetic electrons in a solar flare and compare them with observations. The ultimate goal is to test the viability of the combined MHD/test-particle approach for data-driven modeling of active events in the solar corona and their impact on the heliosphere. Based on an MHD model of X-class solar flare observed on 2017 September 8, we calculate trajectories of a large number of electrons and protons using the relativistic guiding-center approach. Using the obtained particle trajectories, we deduce the spatial and energy distributions of energetic electrons and protons, and calculate bremsstrahlung hard X-ray emission using the “thin-target” approximation. Our approach predicts some key characteristics of energetic particles in the considered flare, including the size and location of the acceleration region, energetic particle trajectories and energy spectra. Most importantly, the hard X-ray bremsstrahlung intensity maps predicted by the model are in good agreement with those observed by RHESSI. Furthermore, the locations of proton and electron precipitation appear to be close to the sources of helioseismic response detected in this flare. Therefore, the adopted approach can be used for observationally driven modeling of individual solar flares, including manifestations of energetic particles in the corona, as well as the inner heliosphere.
Highlights
Observations show that high-energy nonthermal particles may carry a substantial part of the energy released in solar flares
Some of the energetic particles escape from the corona into the heliosphere, and can be observed in situ, usually at 1 au near the Earth, but near the Sun, by Parker Solar Probe (PSP) and Solar Orbiter (SolO) missions
In this study we have investigated particle acceleration and energetic particle transport in the evolving electromagnetic field of an actual solar flare observed in active region NOAA 12673 on 2017 September 6
Summary
Observations show that high-energy nonthermal particles may carry a substantial part of the energy released in solar flares (see, e.g., Aschwanden et al 2016; Kontar et al 2019). Comparison of the energetic electron properties in the corona and near the Earth reveals a strong correlation between their energy spectra and temporal evolution, at least in prompt events (e.g., Krucker et al 2007), indicating that both energetic electron populations have the same origin. Still, their properties in the corona and at 1 au appear to indicate that both populations are strongly affected during transport through the corona and the heliosphere. It was almost impossible to distinguish between different effects affecting
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