The plasmoid instability in a confined solar flare. (arXiv:1905.01201v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+MacTaggart_D/0/1/0/all/0/1">David MacTaggart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fletcher_L/0/1/0/all/0/1">Lyndsay Fletcher</a>
Eruptive flares (EFs) are associated with erupting filaments and, in some
models, filament eruption drives flare reconnection. Recently, however,
observations of a confined flare (CF) have revealed all the hallmarks of an EF
(impulsive phase, flare ribbons, etc.) without the filament eruption itself.
Therefore, if the filament is not primarily responsible for impulsive flare
reconnection, what is? In this Letter, we argue, based on mimimal requirements,
that the plasmoid instability is a strong candidate for explaining the
impulsive phase in the observed CF. We present magnetohydrodynamic simulation
results of the nonlinear development of the plasmoid instability, in a model
active region magnetic field geometry, to strengthen our claim. We also discuss
how the ideas described in this Letter can be generalised to other situations,
including EFs.
Eruptive flares (EFs) are associated with erupting filaments and, in some
models, filament eruption drives flare reconnection. Recently, however,
observations of a confined flare (CF) have revealed all the hallmarks of an EF
(impulsive phase, flare ribbons, etc.) without the filament eruption itself.
Therefore, if the filament is not primarily responsible for impulsive flare
reconnection, what is? In this Letter, we argue, based on mimimal requirements,
that the plasmoid instability is a strong candidate for explaining the
impulsive phase in the observed CF. We present magnetohydrodynamic simulation
results of the nonlinear development of the plasmoid instability, in a model
active region magnetic field geometry, to strengthen our claim. We also discuss
how the ideas described in this Letter can be generalised to other situations,
including EFs.
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