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

Smalley

Abstract

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 d 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 patterns8-10. 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.

• Acceptance Date: Feb 27, 2020
• Publication Date: May 13, 2020
• Journal: Nature
• Print ISSN: 1476-4687
• Publisher: Nature Publishing Group
• Pages: 147 - 151
• DOI: https://doi.org/10.1038/s41586-020-2226-8
• Keywords: Stars, Stellar evolution, Time-domain astronomy
• Publisher URL: https://www.nature.com/articles/s41586-020-2226-8#article-info