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

TL;DR

This study combines multi-wavelength observations and modeling to explore the connection between superflares, prominence eruptions, and CMEs in young Sun-like stars, revealing similarities to solar eruptions and implications for planetary atmospheres.

Contribution

It provides the first multi-wavelength observational evidence linking superflares to CMEs in young Sun-like stars, supporting solar-stellar eruption similarities and advancing models for planetary atmospheric effects.

Findings

Four superflares linked to prominence eruptions

Eruptions associated with potential coronal dimming in X-rays

Solar MHD models support eruption origins from active regions

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.