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. 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 and Roland K. Vanderspek
Additional contact information
Timothy R. Bedding: University of Sydney
Simon J. Murphy: University of Sydney
Daniel R. Hey: University of Sydney
Daniel Huber: University of Hawai‘i
Tanda Li: University of Sydney
Barry Smalley: Keele University
Dennis Stello: Aarhus University
Timothy R. White: University of Sydney
Warrick H. Ball: Aarhus University
William J. Chaplin: Aarhus University
Isabel L. Colman: University of Sydney
Jim Fuller: TAPIR, California Institute of Technology
Eric Gaidos: University of Hawai‘i
Daniel R. Harbeck: Las Cumbres Observatory Global Telescope
J. J. Hermes: Boston University
Daniel L. Holdsworth: University of Central Lancashire
Gang Li: University of Sydney
Yaguang Li: University of Sydney
Andrew W. Mann: University of North Carolina at Chapel Hill
Daniel R. Reese: LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris
Sanjay Sekaran: Instituut voor Sterrenkunde (IvS), KU Leuven
Jie Yu: Max-Planck-Institut für Sonnensystemforschung
Victoria Antoci: Aarhus University
Christoph Bergmann: University of New South Wales
Timothy M. Brown: Las Cumbres Observatory Global Telescope
Andrew W. Howard: TAPIR, California Institute of Technology
Michael J. Ireland: The Australian National University
Howard Isaacson: University of California at Berkeley
Jon M. Jenkins: NASA Ames Research Center
Hans Kjeldsen: Aarhus University
Curtis McCully: Las Cumbres Observatory Global Telescope
Markus Rabus: Las Cumbres Observatory Global Telescope
Adam D. Rains: The Australian National University
George R. Ricker: Massachusetts Institute of Technology
Christopher G. Tinney: University of New South Wales
Roland K. Vanderspek: Massachusetts Institute of Technology

Nature, 2020, vol. 581, issue 7807, 147-151

Abstract: 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.

Date: 2020
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DOI: 10.1038/s41586-020-2226-8

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