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Radio burst from a stellar coronal mass ejection

Nature volume 647, pages 603–607 (2025)Cite this article

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Abstract

Coronal mass ejections (CMEs) are massive expulsions of magnetized plasma from a star and are the largest contributors to space weather in the Solar System1,2. CMEs play an important role in planetary atmospheric erosion, especially for planets that are close to their host star3,4,5. However, this conclusion remains controversial as there has not been an unambiguous detection of a CME from a star outside our Sun. Previous stellar CME studies have only inferred the presence of a CME through the detection of other types of stellar eruptive event6,7,8,9. A signature of a fast CME is a type II radio burst10,11, which is emitted from the shock wave produced as the CME travels through the stellar corona into interplanetary space. Here we report an analogue to a type II burst from the early M dwarf StKM 1-1262. The burst exhibits identical frequency, time and polarization properties to fundamental plasma emission from a solar type II burst. We demonstrate that the rate of these events with similar radio luminosity from M dwarfs is \(0.8{4}_{-0.69}^{+1.94}\times 1{0}^{-3}\) per day per star. Our detection implies that we are no longer restricted to extrapolating the solar CME kinematics and rates to other stars, allowing us to establish observational limits on the impact of CMEs on exoplanets.

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Fig. 1: Dynamic spectra of the burst for different polarizations and durations.
Fig. 2: A ridge-crawler fit to the two different emission lanes evident in the circularly polarized burst.
Fig. 3: Circularly polarized dirty map of StKM 1-1262, imaged over the duration of 2 min burst.

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Data availability

LOFAR visibilities taken are publicly available in the LOFAR Long Term Archive (ObsID: 470106; LoTSS field: P236+53). The XMM-Newton data are available through the XMM-Newton Science Archive (XSA) (ObsID: 0401270201). All other data used in the manuscript have been sourced from the public domain.

Code availability

The important codes used to analyse and process the LOFAR data are available at the following sites: WSClean (https://gitlab.com/aroffringa/wsclean), DynSpecMS (https://github.com/cyriltasse/DynSpecMS) and DDF pipeline (https://github.com/mhardcastle/ddf-pipeline). The posteriors obtained from fitting a geometric flare model to the dynamic radio spectrum are available at GitHub (https://github.com/robkavanagh/papers/tree/main/type-II).

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Acknowledgements

J.R.C. is grateful to J. A. Callingham for her lifelong support. We thank R. Osten and A. Kumari for their useful comments. J.R.C. acknowledges funding from the European Union through the European Research Council (ERC) grant Epaphus (project no. 101166008). R.D.K. and H.K.V. acknowledge funding from the Dutch Research Council (NWO) for the project ‘e-MAPS’ (project no. Vi.Vidi.203.093) under the NWO talent scheme VIDI. S. Bellotti acknowledges funding by the NWO under the project ‘Exo-space weather and contemporaneous signatures of star-planet interactions’ (with project no. OCENW.M.22.215 of the research programme ‘Open Competition Domain Science – M’). P. Zarka acknowledges funding from the ERC under the Horizon 2020 research and innovation programme of the European Union (grant agreement no. 101020459 – Exoradio). H.R. acknowledges the UKSA grant ST/X002012/1 and the STFC grant ST/W001004/1. The LOFAR data in this study were (partly) processed by the LoTSS team. This team made use of the LOFAR direction-independent calibration pipeline (https://github.com/lofar-astron/prefactor), which was deployed by the LOFAR e-infragroup on the Dutch National Grid infrastructure with support of the SURF Co-operative through grants e-infra 170194 and e-infra 180169. The LoTSS direction-dependent calibration and imaging pipeline (http://github.com/mhardcastle/ddf-pipeline/) was run on compute clusters at Leiden Observatory and the University of Hertfordshire, which are supported by a European Research Council advanced grant (NEWCLUSTERS-321271) and the UK Science and Technology Funding Council (ST/P000096/1). The Jülich LOFAR Long Term Archive and the German LOFAR network are both coordinated and operated by the Jülich Supercomputing Centre (JSC), and computing resources on the supercomputer JUWELS at JSC were provided by the Gauss Centre for Supercomputing (grant CHTB00) through the John von Neumann Institute for Computing (NIC).

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Authors and Affiliations

  1. ASTRON, Netherlands Institute for Radio Astronomy, Dwingeloo, The Netherlands

    J. R. Callingham, R. D. Kavanagh, H. K. Vedantham, S. Bloot, D. C. Konijn, T. W. Shimwell & P. Zucca

  2. Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, The Netherlands

    J. R. Callingham & R. D. Kavanagh

  3. LUX, Observatoire de Paris, Université PSL, CNRS, Meudon, France

    C. Tasse

  4. Centre for Radio Astronomy Techniques and Technologies (RATT), Department of Physics and Electronics, Rhodes University, Makhanda, South Africa

    C. Tasse

  5. Observatoire Radioastronomique de Nançay (ORN), Observatoire de Paris, CNRS, PSL, Université d’Orléans, OSUC, Nançay, France

    C. Tasse, P. Zarka & L. Lamy

  6. Max Planck Institute for Solar System Research, Göttingen, Germany

    R. Keers

  7. Faculty of Electrical Engineering, Information Technology, and Physics, Technische Universität Braunschweig, Braunschweig, Germany

    R. Keers

  8. Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands

    H. K. Vedantham, S. Bloot & D. C. Konijn

  9. LIRA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, Meudon, France

    P. Zarka & L. Lamy

  10. Leiden Observatory, Leiden University, Leiden, The Netherlands

    S. Bellotti, H. J. A. Röttgering & T. W. Shimwell

  11. Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, Toulouse, France

    S. Bellotti

  12. Center for Astrophysics, Harvard & Smithsonian, Cambridge, MA, USA

    P. I. Cristofari & E. K. Pass

  13. Centre for Astrophysics Research, University of Hertfordshire, Hatfield, UK

    M. J. Hardcastle

  14. LAM, Aix-Marseille Université, CNRS, CNES, Marseille, France

    L. Lamy

  15. Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA

    E. K. Pass

  16. Department of Physics and Astronomy, Macquarie University, Sydney, New South Wales, Australia

    B. J. S. Pope

  17. Mullard Space Science Laboratory, University College London, Dorking, UK

    H. Reid

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Contributions

J.R.C. initiated the LOFAR project that led to the discovery of the source, conducted the cross-matching analysis and wrote the paper. C.T. wrote the dynamic spectra software and helped interpret the data. R.K. identified the burst. H.K.V., J.R.C., R.D.K. and P. Zarka led the theoretical interpretation of the detection and contributed substantially to the paper. S. Bellotti and P.I.C. obtained the Zeeman Doppler imaging data on the star. M.J.H. and T.W.S. processed the survey data. P. Zucca and H.R. provided solar physics expertise for interpreting the burst. S. Bloot, D.C.K., L.L., E.K.P. and B.J.S.P. commented on the paper and provided optical expertise in characterizing StKM 1-1262. H.J.A.R. is the principal investigator of LoTSS and commented on the paper.

Corresponding authors

Correspondence to J. R. Callingham or C. Tasse.

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Nature thanks Anshu Kumari and the other, anonymous, reviewer(s) for their contribution to the peer review of this work. Peer reviewer reports are available.

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Extended data figures and tables

Extended Data Fig. 1 Reconstruction of the burst assuming ECMI from a high-latitude coronal loop.

While the overall drift rate is recovered, it is not possible to recover the observed sub-structure in Fig. 1.

Extended Data Table 1 Fit parameters for the ECMI emission model
Full size table

Supplementary information

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Callingham, J.R., Tasse, C., Keers, R. et al. Radio burst from a stellar coronal mass ejection. Nature 647, 603–607 (2025). https://doi.org/10.1038/s41586-025-09715-3

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