Gravity-mode main-sequence asteroseismology of 16 open clusters and associations

@misc{li2026gravitymode,
  title = {{Gravity-mode main-sequence asteroseismology of 16 open clusters and associations}},
  author = {Gang Li and Haotian Wang and Anuj Gautam and J. S. G. Mombarg and Simon J. Murphy and Mara Bernizzoni and Mingjie Jian and Saakshi Wadhwa and Dario J. Fritzewski and Facundo D. Moyano and Prasad Mani and Chenyuan Li and Timothy R. Bedding and Conny Aerts},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.25944},
  eprint = {2610.25944},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.25944},
  note = {CC BY 4.0},
}

TY  - UNPB
TI  - Gravity-mode main-sequence asteroseismology of 16 open clusters and associations
AU  - Gang Li
AU  - Haotian Wang
AU  - Anuj Gautam
AU  - J. S. G. Mombarg
AU  - Simon J. Murphy
AU  - Mara Bernizzoni
AU  - Mingjie Jian
AU  - Saakshi Wadhwa
AU  - Dario J. Fritzewski
AU  - Facundo D. Moyano
AU  - Prasad Mani
AU  - Chenyuan Li
AU  - Timothy R. Bedding
AU  - Conny Aerts
PY  - 2026
DA  - 2026/10/19
PB  - arXiv
DO  - 10.48550/arxiv.2610.25944
UR  - https://arxiv.org/abs/2610.25944
AB  - Coeval stellar populations offer a unique advantage for studying stellar physics because their members share a common age and broadly similar initial chemical composition, allowing the free parameters in stellar models to be constrained more efficiently. Meanwhile, asteroseismology, through the study of pulsation modes that propagate through stellar interiors, provides powerful constraints on internal structure and the physical processes operating beneath stellar atmospheres. The combination of coeval-population studies and asteroseismology therefore provides an unparalleled laboratory for testing and improving stellar evolutionary and structural models. Using light curves from the Kepler and TESS space missions, together with membership constraints based on Gaia astrometry, we identify g-mode period-spacing patterns in dozens of early-type (T_eff ≳ 7000 K) main-sequence stars across 16 stellar groups. From these patterns, we infer near-core rotation rates f_rot and measure the asymptotic spacing Π_0 of g modes, tracing both angular-momentum transport and the evolution of the convective stellar cores. Using our homogeneous set of g-mode stellar-group members spanning a wide range of ages, we show that near-core rotation in early-type stars decreases with stellar evolution. We compare our results with existing model predictions. Our Π_0 measurements still show discrepancies with current stellar models for reasons that remain unclear, as reported in several previous studies. We also report two g-mode pre-main-sequence pulsators and three pulsating blue stragglers. Our sample provides a useful basis for calibrating stellar models in future ensemble asteroseismic studies of coeval stellar populations.
ER  -