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Modeling Stellar Winds and Coronal Emission of Young Solar Analogues

Presentation #202.05 in the session Coronal Magnetic Fields and Solar Wind Formation.

Published onSep 18, 2023
Modeling Stellar Winds and Coronal Emission of Young Solar Analogues

In previous work we have employed a surface flux transport (SFT) model to examine the emergence and dynamics of magnetic flux on the surfaces of cool stars like the Sun and other exoplanet host stars of interest. In particular, the class of young active G-type stars can provide clues about the past activity of our own Sun and its effects on the evolution of the solar system planets. Here we present results combining the SFT treatment with the empirical Wang Sheeley Arge (WSA) model for the solar wind to investigate the dependence of solar/stellar wind properties on stellar magnetic activity. Additionally, we employ a coronal heating model to investigate the X-ray and EUV emission of young Sun-like stars. An understanding of the enhanced solar wind driving and XUV emission of active G-type stars can inform the atmospheric loss history of the Earth, or indeed of exoplanets around other Sun-like stars.

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