Volume 606, October 2017
|Number of page(s)||10|
|Published online||16 October 2017|
The association of a J-burst with a solar jet⋆
1 School of Physics, Trinity College Dublin, Dublin 2, Ireland
2 ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA Dwingeloo, The Netherlands
3 School of Physics and Astronomy, SUPA, University of Glasgow, Glasgow G12 8QQ, UK
4 Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
5 RAL Space, Science and Technology Facilities Council, Rutherford Appleton Laboratory, Harwell Campus, Oxfordshire, OX11 OQX, UK
6 Solar-Terrestrial Center of Excellence, SIDC, Royal Observatory of Belgium, Avenue Circulaire 3, 1180 Brussels, Belgium
7 Commission for Astronomy, Austrian Academy of Sciences, Schmiedlstrasse 6, 8042 Graz, Austria
8 Swedish Institute of Space Physics, Box 537, 75121 Uppsala, Sweden
9 Helmholtz-Zentrum Potsdam, DeutschesGeoForschungsZentrum GFZ, Department 1: Geodesy and Remote Sensing, Telegrafenberg, A17, 14473 Potsdam, Germany
10 Shell Technology Center, 562149 Bangalore, India
11 SRON Netherlands Insitute for Space Research, PO Box 800, 9700 AV Groningen, The Netherlands
12 Kapteyn Astronomical Institute, PO Box 800, 9700 AV Groningen, The Netherlands
13 CSIRO Astronomy and Space Science, 26 Dick Perry Avenue, Kensington, WA 6151, Australia
14 University of Twente, 75222 Enshed, The Netherlands
15 Institute for Astronomy, University of Edinburgh, Royal Observatory of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK
16 University of Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany
17 Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, 85741 Garching, Germany
18 SmarterVision BV, Oostersingel 5, 9401 JX Assen, The Netherlands
19 Thüringer Landessternwarte, Sternwarte 5, 07778 Tautenburg, Germany
20 Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
21 Jodrell Bank Center for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester M13 9PL, UK
22 Leiden Observatory, Leiden University, PO Box9513, 2300 RA Leiden, The Netherlands
23 LPC2E – Université d’Orléans/CNRS, 45071 Orléans Cedex, France
24 Station de Radioastronomie de Nançay, Observatoire de Paris – CNRS/INSU, USR 704 – Univ. Orléans, OSUC, route de Souesmes, 18330 Nançay, France
25 Astronomisches Institut der Ruhr-Universität Bochum, Universitaetsstrasse 150, 44780 Bochum, Germany
26 Sodankylä Geophysical Observatory, University of Oulu, Tähteläntie 62, 99600 Sodankylä, Finland
27 STFC Rutherford Appleton Laboratory, Harwell Science and Innovation Campus, Didcot OX11 0QX, UK
28 Radboud University Radio Lab, Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
29 Department of Physics and Astronomy, University of California Irvine, Irvine, CA 92697, USA
30 Center for Information Technology (CIT), University of Groningen, The Netherlands
31 Centre de Recherche Astrophysique de Lyon, Observatoire de Lyon, 9 Ave. Charles André, 69561 Saint-Genis Laval Cedex, France
32 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
33 Fakultät für Physik, Universität Bielefeld, Postfach 100131, 33501 Bielefeld, Germany
34 Department of Physics and Elelctronics, Rhodes University, PO Box 94, Grahamstown 6140, South Africa
35 SKA South Africa, 3rd Floor, The Park, Park Road, 7405 Pinelands, South Africa
36 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
37 LESIA & USN, Observatoire de Paris, CNRS, PSL/SU/UPMC/UPD/SPC, Place J. Janssen, 92195 Meudon, France
Received: 2 November 2016
Accepted: 11 August 2017
Context. The Sun is an active star that produces large-scale energetic events such as solar flares and coronal mass ejections, and numerous smaller scale events such as solar jets. These events are often associated with accelerated particles that can cause emission at radio wavelengths. The reconfiguration of the solar magnetic field in the corona is believed to be the cause of the majority of solar energetic events and accelerated particles.
Aims. Here, we investigate a bright J-burst that was associated with a solar jet and the possible emission mechanism causing these two phenomena.
Methods. We used data from the Solar Dynamics Observatory (SDO) to observe a solar jet and radio data from the Low Frequency Array (LOFAR) and the Nançay Radioheliograph (NRH) to observe a J-burst over a broad frequency range (33–173 MHz) on 9 July 2013 at ~11:06 UT.
Results. The J-burst showed fundamental and harmonic components and was associated with a solar jet observed at extreme ultraviolet wavelengths with SDO. The solar jet occurred in the northern hemisphere at a time and location coincident with the radio burst and not inside a group of complex active regions in the southern hemisphere. The jet occurred in the negative polarity region of an area of bipolar plage. Newly emerged positive flux in this region appeared to be the trigger of the jet.
Conclusions. Magnetic reconnection between the overlying coronal field lines and the newly emerged positive field lines is most likely the cause of the solar jet. Radio imaging provides a clear association between the jet and the J-burst, which shows the path of the accelerated electrons. These electrons travelled from a region in the vicinity of the solar jet along closed magnetic field lines up to the top of a closed magnetic loop at a height of ~360 Mm. Such small-scale complex eruptive events arising from magnetic reconnection could facilitate accelerated electrons to produce continuously the large numbers of Type III bursts observed at low frequencies, in a similar way to the J-burst analysed here.
Key words: Sun: corona / Sun: radio radiation / Sun: particle emission / Sun: magnetic fields
© ESO, 2017
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