Solar flare radio pulsations as a signature of dynamic magnetic reconnection

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dc.creatorKliem, B.
dc.creatorKarlicky, M.
dc.creatorBenz, A. O.
dc.date2000-06-22
dc.date.accessioned2026-07-07T01:54:06Z
dc.date.available2026-07-07T01:54:06Z
dc.descriptionDecimetric radio observations of the impulsive solar flare on October 5, 1992, 09:25 UT show a long series of quasi-periodic pulsations deeply modulating a continuum in the 0.6-2 GHz range that is slowly drifting toward lower frequencies. We propose a model in which the pulsations of the radio flux are caused by quasi-periodic particle acceleration episodes that result from a dynamic phase of magnetic reconnection in a large-scale current sheet. The reconnection is dominated by repeated formation and subsequent coalescence of magnetic islands (known as ``secondary tearing'' or ``impulsive bursty'' regime of reconnection), while a continuously growing plasmoid is fed by newly coalescing islands. Such a model, involving a current sheet and a growing plasmoid, is consistent with the Yohkoh observations of the same flare (Ohyama & Shibata 1998). We present two-dimensional MHD simulations of dynamic magnetic reconnection that support the model. Within the framework of the proposed interpretation, the radio observations reveal details of plasmoid formation in flares.
dc.descriptionA file with full-quality figures is available at http://www.aip.de/~preprint/preprints/2000/2000_23.html
dc.identifierhttps://arxiv.org/abs/astro-ph/0006324
dc.identifierhttp://arxiv.org/abs/astro-ph/0006324
dc.identifierAstron.Astrophys. 360 (2000) 715
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/1214
dc.subjectAstrophysics
dc.titleSolar flare radio pulsations as a signature of dynamic magnetic reconnection
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