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

Timothy R. Bedding*, Simon J. Murphy, Daniel R. Hey, Daniel Huber, Tanda Li, Barry Smalley, Dennis Stello, Timothy R. White, Warrick H. Ball, William J. Chaplin, Isabel L. Colman, Jim Fuller, Eric Gaidos, Daniel R. Harbeck, J. J. Hermes, Daniel L. Holdsworth, Gang Li, Yaguang Li, Andrew W. Mann, Daniel R. ReeseSanjay Sekaran, Jie Yu, Victoria Antoci, Christoph Bergmann, Timothy M. Brown, Andrew W. Howard, Michael J. Ireland, Howard Isaacson, Jon M. Jenkins, Hans Kjeldsen, Curtis McCully, Markus Rabus, Adam D. Rains, George R. Ricker, Christopher G. Tinney, Roland K. Vanderspek

*Corresponding author for this work

    Research output: Contribution to journalJournal articleResearchpeer-review

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    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.

    Original languageEnglish
    JournalNature
    Volume581
    Issue number7807
    Pages (from-to)147-151
    ISSN0028-0836
    DOIs
    Publication statusPublished - 2020

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