Speaker
Description
Stars are the fundamental building blocks of the Universe. Their dynamics, nucleosynthesis, and supernova explosions are closely linked to the formation and evolution of the Milky Way, the chemical enrichment of galaxies, and even cosmology. Although modern stellar theory has achieved great success, the physical processes in stellar cores remain highly uncertain because the interior cannot be directly observed by traditional methods, limiting the understanding of stellar evolution theory.
Asteroseismology, the only technique capable of efficiently probing stellar interiors, is playing an increasingly important role in the era of space-based observations. The oscillation modes inside stars are modulated by their internal physical conditions, leading to measurable changes in frequency and amplitude; once these waves reach the surface, they appear as periodic brightness variations. By precisely measuring the oscillation frequencies, we can infer the internal structure and evolutionary state of stars.
In this talk, I will present several recent advances made using Kepler and TESS asteroseismic data. First, among more than 2,000 red giants, we detected magnetism-induced signals in over a dozen stars, yielding magnetic field strengths of 20–150 kG—the most direct evidence of strong internal fields in stars to date. Second, through large-sample analyses of gravity and mixed modes, we constrained the core and envelope rotation rates of thousands of main-sequence and red giant stars, revealing significant discrepancies with theoretical predictions and providing crucial constraints on angular momentum transport mechanisms. Finally, I will show how combining asteroseismic analysis of open clusters (e.g., NGC 2516) with isochrone fitting enables highly precise age determinations, offering a new approach to measuring cluster ages.
| Session Selection | Astronomy and Astrophysics |
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