Authors: Varun Chaturmutha (Georgia State University), Bernhard Fleck (ESA Science and Operations), Stuart Jefferies (Georgia State University)

At the turn of the 21st century, helioseismology was extended to other stars as asteroseismology, emerging as a powerful tool to study physical processes in stellar interiors. While space missions like CoRoT, Kepler, and TESS have enabled us to probe internal properties of stars—such as density, composition, rotation, and convective mixing—stellar atmospheres have remained largely unexplored. Here, we present a groundbreaking approach to probe stellar atmospheres, utilizing multi-height, line-of-sight Doppler velocity observations of the Sun, simulated as if it were a distant star. By analyzing disk-integrated Doppler velocity data from spectral lines formed at different atmospheric heights, such as Na from SOHO/GOLF and Fe from SDO/HMI, we model the propagation of acoustic-gravity waves between these heights. This method, extensively utilized on the Sun’s surface, is adapted here for stellar atmospheres, revealing potential insights into sound speed (temperature), radiative cooling times (energy transport), and magnetic cycles (stellar dynamos). Our results highlight the promise of seismic probing of stellar atmospheres, setting the stage for future investigations into these critical stellar properties.