Low altitude solar magnetic reconnection, type III solar radio bursts and X-ray emissions

Cairns, I. H. ; Lobzin, V. V. ; Donea, A. ; Tingay, S. J. ; McCauley, P. I. ; Oberoi, D. ; Duffin, R. T. ; Reiner, M. J. ; Hurley-Walker, N. ; Kudryavtseva, N. A. ; Melrose, D. B. ; Harding, J. C. ; Bernardi, G. ; Bowman, J. D. ; Cappallo, R. J. ; Corey, B. E. ; Deshpande, A. ; Emrich, D. ; Goeke, R. ; Hazelton, B. J. ; Johnston-Hollitt, M. ; Kaplan, D. L. ; Kasper, J. C. ; Kratzenberg, E. ; Lonsdale, C. J. ; Lynch, M. J. ; McWhirter, S. R. ; Mitchell, D. A. ; Morales, M. F. ; Morgan, E. ; Ord, S. M. ; Prabu, T. ; Roshi, A. ; Shankar, N. Udaya ; Srivani, K. S. ; Subrahmanyan, R. ; Wayth, R. B. ; Waterson, M. ; Webster, R. L. ; Whitney, A. R. ; Williams, A. ; Williams, C. L. (2018) Low altitude solar magnetic reconnection, type III solar radio bursts and X-ray emissions Scientific Reports, 8 (1). Article ID 1676-12 pages. ISSN 2045-2322

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Official URL: https://www.nature.com/articles/s41598-018-19195-3

Related URL: http://dx.doi.org/10.1038/s41598-018-19195-3


Type III solar radio bursts are the Sun’s most intense and frequent nonthermal radio emissions. They involve two critical problems in astrophysics, plasma physics, and space physics: how collective processes produce nonthermal radiation and how magnetic reconnection occurs and changes magnetic energy into kinetic energy. Here magnetic reconnection events are identified definitively in Solar Dynamics Observatory UV-EUV data, with strong upward and downward pairs of jets, current sheets, and cusp-like geometries on top of time-varying magnetic loops, and strong outflows along pairs of open magnetic field lines. Type III bursts imaged by the Murchison Widefield Array and detected by the Learmonth radiospectrograph and STEREO B spacecraft are demonstrated to be in very good temporal and spatial coincidence with specific reconnection events and with bursts of X-rays detected by the RHESSI spacecraft. The reconnection sites are low, near heights of 5–10 Mm. These images and event timings provide the long-desired direct evidence that semi-relativistic electrons energized in magnetic reconnection regions produce type III radio bursts. Not all the observed reconnection events produce X-ray events or coronal or interplanetary type III bursts; thus different special conditions exist for electrons leaving reconnection regions to produce observable radio, EUV, UV and X-ray bursts.

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Deposited On:21 May 2018 08:56
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