Help Privacy Policy Disclaimer
  Advanced SearchBrowse




Journal Article

Very regular high-frequency pulsation modes in young intermediate-mass stars


Yu ,  Jie
Max Planck Institute for Solar System Research, Max Planck Society;

External Resource
No external resources are shared
Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available

Bedding, T. R., Murphy, S. J., Hey, D. R., Huber, D., Li, T., Smalley, B., et al. (2020). Very regular high-frequency pulsation modes in young intermediate-mass stars. Nature, 581(7807), 147-151. doi:10.1038/s41586-020-2226-8.

Cite as: https://hdl.handle.net/21.11116/0000-0006-9F3D-4
Asteroseismology probes the internal structures of stars by using their natural pulsation frequencies1. It relies on identifying sequences of pulsation modes that can be compared with theoretical models, which has been done successfully for many classes of pulsators, including low-mass solar-type stars2, red giants3, high-mass stars4 and white dwarfs5. However, a large group of pulsating stars of intermediate mass—the so-called δ Scuti stars—have rich pulsation spectra for which systematic mode identification has not hitherto been possible6,7. This arises because only a seemingly random subset of possible modes are excited and because rapid rotation tends to spoil regular patterns8,9,10. Here we report the detection of remarkably regular sequences of high-frequency pulsation modes in 60 intermediate-mass main-sequence stars, which enables definitive mode identification. The space motions of some of these stars indicate that they are members of known associations of young stars, as confirmed by modelling of their pulsation spectra.