Cairns, I. H.I. H.CairnsLobzin, V. V.V. V.LobzinDonea, A.A.DoneaTingay, S. J.S. J.TingayMcCauley, P. I.P. I.McCauleyOberoi, D.D.OberoiDuffin, R. T.R. T.DuffinReiner, M. J.M. J.ReinerHurley-Walker, N.N.Hurley-WalkerKudryavtseva, N. A.N. A.KudryavtsevaMelrose, D. B.D. B.MelroseHarding, J. C.J. C.HardingBERNARDI, GIANNIGIANNIBERNARDIBowman, J. D.J. D.BowmanCappallo, R. J.R. J.CappalloCorey, B. E.B. E.CoreyDeshpande, A.A.DeshpandeEmrich, D.D.EmrichGoeke, R.R.GoekeHazelton, B. J.B. J.HazeltonJohnston-Hollitt, M.M.Johnston-HollittKaplan, D. L.D. L.KaplanKasper, J. C.J. C.KasperKratzenberg, E.E.KratzenbergLonsdale, C. J.C. J.LonsdaleLynch, M. J.M. J.LynchMcWhirter, S. R.S. R.McWhirterMitchell, D. A.D. A.MitchellMorales, M. F.M. F.MoralesMorgan, E.E.MorganOrd, S. M.S. M.OrdPrabu, T.T.PrabuRoshi, A.A.RoshiShankar, N. UdayaN. UdayaShankarSrivani, K. S.K. S.SrivaniSubrahmanyan, R.R.SubrahmanyanWayth, R. B.R. B.WaythWaterson, M.M.WatersonWebster, R. L.R. L.WebsterWhitney, A. R.A. R.WhitneyWilliams, A.A.WilliamsWilliams, C. L.C. L.Williams2020-10-132020-10-1320182045-2322http://hdl.handle.net/20.500.12386/27778Type 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.ELETTRONICOenArticle10.1038/s41598-018-19195-32-s2.0-85041130117000423428300004https://www.nature.com/articles/s41598-018-19195-32018NatSR...8.1676CFIS/05 - ASTRONOMIA E ASTROFISICAERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation