| Literature DB >> 32405022 |
Timothy R Bedding1,2, Simon J Murphy3,4, Daniel R Hey3,4, Daniel Huber5, Tanda Li3,4,6, Barry Smalley7, Dennis Stello4,8, Timothy R White3,4,9, Warrick H Ball4,6, William J Chaplin4,6, Isabel L Colman3,4, Jim Fuller10, Eric Gaidos11, Daniel R Harbeck12, J J Hermes13, Daniel L Holdsworth14, Gang Li3,4, Yaguang Li3,4,15, Andrew W Mann16, Daniel R Reese17, Sanjay Sekaran18, Jie Yu19, Victoria Antoci4,20, Christoph Bergmann8, Timothy M Brown12, Andrew W Howard10, Michael J Ireland9, Howard Isaacson21, Jon M Jenkins22, Hans Kjeldsen4,23, Curtis McCully12, Markus Rabus12,24, Adam D Rains9, George R Ricker25,26, Christopher G Tinney8, Roland K Vanderspek25,26.
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 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 patterns8-10. 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.Year: 2020 PMID： 32405022 DOI： 10.1038/s41586-020-2226-8
Source DB: PubMed Journal: Nature ISSN： 0028-0836 Impact factor: 49.962