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

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

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Authors

Timothy R. Bedding

Simon J. Murphy

Daniel R. Hey

Daniel Huber

Tanda Li

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. Reese

Sanjay 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



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.

Journal Article Type Article
Acceptance Date Feb 27, 2020
Online Publication Date May 13, 2020
Publication Date May 14, 2020
Publicly Available Date May 26, 2023
Journal Nature
Print ISSN 1476-4687
Publisher Nature Publishing Group
Peer Reviewed Peer Reviewed
Volume 581
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

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