Beam electrons as a source of Hα flare ribbons

Malcolm Druett (), Eamon Scullion, Valentina Zharkova, Sarah Matthews, Sergei Zharkov and Luc Rouppe Van der Voort
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Malcolm Druett: Northumbria University, Physics and Electrical Engineering
Eamon Scullion: Northumbria University, Physics and Electrical Engineering
Valentina Zharkova: Northumbria University, Physics and Electrical Engineering
Sarah Matthews: Mullard Space Science Laboratory, University College London
Sergei Zharkov: Hull University, School of Mathematics & Physical Sciences
Luc Rouppe Van der Voort: Institute of Theoretical Astrophysics, University of Oslo

Nature Communications, 2017, vol. 8, issue 1, 1-13

Abstract: Abstract The observations of solar flare onsets show rapid increase of hard and soft X-rays, ultra-violet emission with large Doppler blue shifts associated with plasma upflows, and Hα hydrogen emission with red shifts up to 1–4 Å. Modern radiative hydrodynamic models account well for blue-shifted emission, but struggle to reproduce closely the red-shifted Hα lines. Here we present a joint hydrodynamic and radiative model showing that during the first seconds of beam injection the effects caused by beam electrons can reproduce Hα line profiles with large red-shifts closely matching those observed in a C1.5 flare by the Swedish Solar Telescope. The model also accounts closely for timing and magnitude of upward motion to the corona observed 29 s after the event onset in 171 Å by the Atmospheric Imaging Assembly/Solar Dynamics Observatory.

Date: 2017
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DOI: 10.1038/ncomms15905

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