Tracking of an electron beam through the solar corona with LOFAR

G. Mann 1 F. Breitling 1 C. Vocks 1 H. Aurass M. Steinmetz 2 G. Strassmeier M. Bisi 3 R. Fallows 4 P. Gallagher A. Kerdraon 5 A. Mackinnon 6 J. Magdalenic 7 H. Rucker 8 J. Anderson 9 A. Asgekar 10 M. Avruch 11 M. Bell 12 J. Bentum G. Bernardi 13 P. Best 14 L. Bîrzan 15 A. Bonafede 16 J. Broderick 17 M. Brüggen 18 R. Butcher B. Ciardi 19 A. Corstanje 20 F. De Gasperin E. Geus A. Deller 21 S. Duscha 10 J. Eislöffel 22 D. Engels 23 H. Falcke 24 R. Fender 25 C. Ferrari 26 W. Frieswijk 10 M. Garrett 15 Jean-Mathias Grießmeier 27, 28, 5 A. Gunst 21 M. Haarlem E. Hassall 29 G. Heald 21 J. T. Hessels M. Hoeft 30 J. Horandel 20 A. Horneffer 9 E. Juette 31 A. Karastergiou 25 A. A. Klijn V. Kondratiev M. Kramer 9 M. Kuniyoshi 9 G. Kuper 10 P. Maat 10 S. Markoff 32 R. Mcfadden 33 D. Mckay-Bukowski 34 J. Mckean 21 D. Mulcahy 35 H. Munk 33 A. Nelles 20 J. Norden E. Orru 10 H. Paas 36 M. Pandey V. Pandey 37 R. Pizzo 10 A. Polatidis 21 D. Rafferty 15 W. Reich 9 H. Röttgering 15 M. M. Scaife J. Schwarz M. Serylak 25 J. Sluman 10 O. Smirnov 38 B. Stappers 35 Michel Tagger 27 Y. Tang 10 C. Tasse 5 S. Veen S. Thoudam 20 M. Toribio R. Vermeulen 10 J. Weeren M. Wise 32 O. Wucknitz 39 S. Yatawatta 21 P. Zarka 5 J. Zensus
Abstract : The Sun's activity leads to bursts of radio emission, among other phenomena. An example is type-III radio bursts. They occur frequently and appear as short-lived structures rapidly drifting from high to low frequencies in dynamic radio spectra. They are usually interpreted as signatures of beams of energetic electrons propagating along coronal magnetic field lines. Here we present novel interferometric LOFAR (LOw Frequency ARray) observations of three solar type-III radio bursts and their reverse bursts with high spectral, spatial, and temporal resolution. They are consistent with a propagation of the radio sources along the coronal magnetic field lines with nonuniform speed. Hence, the type-III radio bursts cannot be generated by a monoenergetic electron beam, but by an ensemble of energetic electrons with a spread distribution in velocity and energy. Additionally, the density profile along the propagation path is derived in the corona. It agrees well with three-fold coronal density model by (1961, ApJ, 133, 983).
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G. Mann, F. Breitling, C. Vocks, H. Aurass, M. Steinmetz, et al.. Tracking of an electron beam through the solar corona with LOFAR. Astronomy and Astrophysics - A&A, EDP Sciences, 2018, 611, pp.Article number A57. ⟨10.1051/0004-6361/201629017⟩. ⟨insu-01897905⟩

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