Magnetic reconnection is a key process that explosively accelerates charged particles, generating phenomena such as nebular flares1, solar flares2 and stunning aurorae3. In planetary magnetospheres, magnetic reconnection has often been identified on the dayside magnetopause and in the nightside magnetodisc, where thin-current-sheet conditions are conducive to reconnection4. The dayside magnetodisc is usually considered thicker than the nightside due to the compression of solar wind, and is therefore not an ideal environment for reconnection. In contrast, a recent statistical study of magnetic flux circulation strongly suggests that magnetic reconnection must occur throughout Saturn’s dayside magnetosphere5. Additionally, the source of energetic plasma can be present in the noon sector of giant planetary magnetospheres6. However, so far, dayside magnetic reconnection has only been identified at the magnetopause. Here, we report direct evidence of near-noon reconnection within Saturn’s magnetodisc using measurements from the Cassini spacecraft. The measured energetic electrons and ions (ranging from tens to hundreds of keV) and the estimated energy flux of ~2.6 mW m2 within the reconnection region are sufficient to power aurorae. We suggest that dayside magnetodisc reconnection can explain bursty phenomena in the dayside magnetospheres of giant planets, which can potentially advance our understanding of quasi-periodic injections of relativistic electrons6 and auroral pulsations7.

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This work was supported by the National Science Foundation of China (41525016, 41474155, 41704169, 41274167 and 41621063). Z.H.Y. is a Marie Curie COFUND research fellow, cofunded by the EU. Cassini operations are supported by NASA (managed by the Jet Propulsion Laboratory) and European Space Agency (ESA). R.L.G. is supported by the opening fund of the Lunar and Planetary Science Laboratory (a partner laboratory of the Key Laboratory of Lunar and Deep Space Exploration) (Macau FDCT grant 039/2013/A2). I.J.R. is supported in part by Science and Technology Facilities Council (STFC) grant ST/N000722/1. Z.H.Y., B.P. and D.G. are supported by the PRODEX programme managed by ESA in collaboration with the Belgian Federal Science Policy Office. W.R.D. is supported by an STFC research grant to University College London, an SAO fellowship to the Harvard–Smithsonian Centre for Astrophysics and ESA contract 4000120752/17/NL/MH. A.J.C. is supported by STFC Consolidated Grants to UCL-MSSL (ST/K000977/1 and ST/N000722/1).

Author information


  1. Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China

    • R. L. Guo
    •  & Y. Wei
  2. Laboratoire de Physique Atmosphérique et Planétaire, STAR Institute, Université de Liège, Liège, Belgium

    • R. L. Guo
    • , Z. H. Yao
    • , D. Grodent
    •  & B. Palmaerts
  3. College of Earth and Planetary Sciences, University of Chinese Academy of Sciences, Beijing, China

    • Y. Wei
  4. Department of Physics, Lancaster University, Lancaster, UK

    • L. C. Ray
    •  & C. S. Arridge
  5. Mullard Space Science Laboratory, University College London, Dorking, UK

    • I. J. Rae
    • , A. J. Coates
    •  & W. R. Dunn
  6. University of Alaska Fairbanks, Geophysical Institute, Fairbanks, AK, USA

    • P. A. Delamere
  7. Office for Space Research and Technology, Academy of Athens, Athens, Greece

    • N. Sergis
  8. Institute of Astronomy, Astrophysics, Space Applications and Remote Sensing, National Observatory of Athens, Athens, Greece

    • N. Sergis
  9. Applied Physics Laboratory, Johns Hopkins University, Laurel, MD, USA

    • P. Kollmann
  10. Southwest Research Institute, San Antonio, TX, USA

    • J. H. Waite
    •  & J. L. Burch
  11. School of Earth and Space Sciences, Peking University, Beijing, China

    • Z. Y. Pu
  12. Department of Physics, Faculty of Natural Sciences, Imperial College, London, UK

    • M. K. Dougherty


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All authors were involved in writing the paper. R.L.G., Z.H.Y. and Y.W. led the work and conducted most of the analysis for the Cassini measurements. L.C.R. provided knowledge of planetary magnetospheric dynamics and critical review of the techniques applied, along with extensive paper writing and data analysis. I.J.R., C.S.A., P.A.D., Z.Y.P. and J.L.B. provided expertise on auroral drivers and magnetospheric processes. N.S. and P.K. provided crucial support in using ion data, as well as insight on magnetospheric dynamics. A.J.C., D.G., W.R.D., J.H.W., B.P. and M.K.D. provided detailed knowledge of planetary magnetospheres.

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Correspondence to Z. H. Yao.

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