The 22nd Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (San Diego, June 2024)
Published July 27, 2024 | Version v1
Presentation Open

Coronal Mass Ejections on Young Suns: Insights from Solar and Stellar Observations and Models

Authors/Creators

  • 1. ROR icon Kyoto University
  • 2. ROR icon National Astronomical Observatory of Japan

Contributors

  • 1. American University
  • 2. NASA Goddard Space Flight Center
  • 3. Observatoire Midi-Pyrénées
  • 4. ROR icon National Astronomical Observatory of Japan
  • 5. ROR icon The University of Tokyo
  • 6. ROR icon Kyoto University
  • 7. Laboratory for Atmospheric and Space Physics
  • 8. ROR icon National Solar Observatory
  • 9. ROR icon Goddard Space Flight Center
  • 10. University of Maryland
  • 11. Bulgarian Academy of Sciences
  • 12. Max Planck Institute
  • 13. University of Southern Queensland
  • 14. Université de Montpellier
  • 15. Paris Observatory
  • 16. ROR icon Leiden University
  • 17. ROR icon Doshisha University

Description

Recent discoveries have revealed exoplanets orbiting young Sun-like stars, offering a window into the early solar system. The young stars are known to produce extreme magnetic explosions, called superflares, about once a day, potentially triggering fast and massive coronal mass ejections (CMEs). Recent studies suggest such ejections could induce atmospheric loss and chemical reactions in early exoplanet atmospheres. However, the association of CMEs with superflares is still unexplored. Here we present the results of 5-years multi-wavelength observations of young Sun-like stars, providing the critical clues to the common picture of solar and stellar CMEs. First, through optical spectroscopic observations, we found four of eleven superflares are associated with fast prominence eruptions, precursors to CMEs. The stellar data greatly resemble solar counterparts, indicating a common picture of solar/stellar eruptions. Second, one of the eruptions is associated with potential coronal dimming in X-rays, indicating that the prominence eruptions evolved into stellar CMEs propagating through interplanetary space. Furthermore, the extension of solar MHD model supports the above indication and suggests that the eruption originates from the observed magnetic active region. This comprehensive study suggests that further advancing the use of solar model could provide the first empirical inputs into calculations of atmospheric escape and chemical reactions for young planets.

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Additional details

References

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