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

Kosuke Namekata

TL;DR

The study investigates coronal mass ejections from young Sun-like stars to understand early solar-system space weather. It employs a five-year, multi-wavelength campaign combining optical spectroscopy, TESS photometry, NICER X-ray monitoring, and Zeeman-Doppler imaging to detect filament and prominence eruptions and coronal dimming as CME signatures. The results show superflares on young Sun-like stars are linked to fast, massive, solar-like eruptions, supported by multi-wavelength signatures and data-driven MHD modeling. The inferred CME activity implies non-negligible mass loss that can affect planetary atmospheres and stellar angular momentum evolution, providing empirical inputs for atmospheric escape and chemical-reaction modeling in young planetary systems.

Abstract

Recent discoveries have revealed exoplanets orbiting young Sun-like stars, offering a window into the early solar system. These young stars frequently produce extreme magnetic explosions known as superflares, roughly once a day, potentially leading to fast and massive coronal mass ejections (CMEs). Recent research have highlighted the importance of stellar CMEs, as these events and associated particles can trigger atmospheric loss and initiate chemical reactions in planetary atmospheres. However, the observation of these associated CMEs remains largely unexplored, marking a crucial first step in assessing the particle environment. 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 fifteen 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 active region inferred by Zeeman Doppler Imaging and TESS light curve modeling. This comprehensive study suggests that further advancing the use of solar model could provide the first empirical inputs into calculations of atmospheric escape/chemical reactions for young planets.

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

TL;DR

The study investigates coronal mass ejections from young Sun-like stars to understand early solar-system space weather. It employs a five-year, multi-wavelength campaign combining optical spectroscopy, TESS photometry, NICER X-ray monitoring, and Zeeman-Doppler imaging to detect filament and prominence eruptions and coronal dimming as CME signatures. The results show superflares on young Sun-like stars are linked to fast, massive, solar-like eruptions, supported by multi-wavelength signatures and data-driven MHD modeling. The inferred CME activity implies non-negligible mass loss that can affect planetary atmospheres and stellar angular momentum evolution, providing empirical inputs for atmospheric escape and chemical-reaction modeling in young planetary systems.

Abstract

Recent discoveries have revealed exoplanets orbiting young Sun-like stars, offering a window into the early solar system. These young stars frequently produce extreme magnetic explosions known as superflares, roughly once a day, potentially leading to fast and massive coronal mass ejections (CMEs). Recent research have highlighted the importance of stellar CMEs, as these events and associated particles can trigger atmospheric loss and initiate chemical reactions in planetary atmospheres. However, the observation of these associated CMEs remains largely unexplored, marking a crucial first step in assessing the particle environment. 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 fifteen 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 active region inferred by Zeeman Doppler Imaging and TESS light curve modeling. This comprehensive study suggests that further advancing the use of solar model could provide the first empirical inputs into calculations of atmospheric escape/chemical reactions for young planets.
Paper Structure (7 sections, 3 figures)

This paper contains 7 sections, 3 figures.

Table of Contents

  1. Introduction
  2. Discovery of Stellar Filament Eruptions
  3. Multiwavelength Signatures of Stellar CMEs
  4. Data-Driven Models
  5. Magnetic Environment of Eruptions
  6. Frequency and CME-Driven Mass Loss
  7. Summary and Conclusion

Figures (3)

  • Figure 1: Dynamic spectrum of H$\alpha$ line. Left: filament eruption (blueshifted absorption, adapted from 2022NatAs...6..241N); Right: prominence eruption (blueshifted emission, 2024ApJ...961...23N)
  • Figure 2: (a,b) Assumed geometry in a pseudo 2D MHD model of magnetic loop expantion (black lines) and prominence material (orange). (c) Simulated H$\alpha$ dynamic spectrum.
  • Figure 3: Starspot maps when the prominence eruption in Figure \ref{['fig:1']} (right) occurred, showing the Doppler imaging (green) and those from the TESS light-curve modeling (gray circles), the radial magnetic field (red and blue colors).