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

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dc.contributor.authorBedding, Timothy Russell
dc.contributor.authorMurphy, Simon
dc.contributor.authorHey, Daniel R.
dc.contributor.authorHuber, Daniel
dc.contributor.authorLi, Tanda
dc.contributor.authorSmalley, B.
dc.contributor.authorStello, Dennis
dc.contributor.authorWhite, Timothy
dc.contributor.authorBall, Warrick
dc.contributor.authorChaplin, W. J.
dc.contributor.authorColman, Isabel L.
dc.contributor.authorIreland, Michael
dc.contributor.authorRains, Adam
dc.date.accessioned2023-08-07T00:13:21Z
dc.date.issued2020-05-13
dc.date.updated2021-08-01T08:22:44Z
dc.description.abstractAsteroseismology 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 patterns8,9,10. 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.en_AU
dc.description.sponsorshipThis research was partially conducted during the Exostar19 programme at the Kavli Institute for Theoretical Physics at UC Santa Barbara, which was supported in part by the National Science Foundation under grant no. NSF PHY-1748958. We gratefully acknowledge support from the Australian Research Council (grant DE 180101104), and from the Danish National Research Foundation (grant DNRF106) through its funding for the Stellar Astrophysics Center (SAC). D.H. acknowledges support from the Alfred P. Sloan Foundation, the National Aeronautics and Space Administration (80NSSC18K1585, 80NSSC19K0379), and the National Science Foundation (AST-1717000). H.K. acknowledges support from the European Social Fund via the Lithuanian Science Council (LMTLT) grant 09.3.3-LMT-K-712-01-0103. Y.L. acknowledges support from the Joint Research Fund in Astronomy (U1631236) under cooperative agreement between the National Natural Science Foundation of China (NSFC) and Chinese Academy of Sciences (CAS). D.L.H. acknowledges support by the Science and Technology Facilities Council under grant ST/M000877/1. The research leading to these results has (partially) received funding from the Research Foundation Flanders (FWO) under grant agreement G0H5416N (ERC Runner Up Project).en_AU
dc.format.mimetypeapplication/pdfen_AU
dc.identifier.citationBedding, T.R., Murphy, S.J., Hey, D.R. et al. Very regular high-frequency pulsation modes in young intermediate-mass stars. Nature 581, 147–151 (2020). https://doi.org/10.1038/s41586-020-2226-8en_AU
dc.identifier.issn0028-0836en_AU
dc.identifier.urihttp://hdl.handle.net/1885/294824
dc.language.isoen_AUen_AU
dc.publisherMacmillan Publishers Ltden_AU
dc.relationhttp://purl.org/au-research/grants/arc/DE180101104en_AU
dc.rights© 2020 The authorsen_AU
dc.sourceNatureen_AU
dc.titleVery regular high-frequency pulsation modes in young intermediate-mass starsen_AU
dc.typeJournal articleen_AU
dcterms.dateAccepted2020-02-27
local.bibliographicCitation.issue7807en_AU
local.bibliographicCitation.lastpage151en_AU
local.bibliographicCitation.startpage147en_AU
local.contributor.affiliationBedding, Timothy Russell, University of Sydneyen_AU
local.contributor.affiliationMurphy, Simon, The University of Sydneyen_AU
local.contributor.affiliationHey, Daniel R., University of Sydneyen_AU
local.contributor.affiliationHuber, Daniel, University of Hawaiien_AU
local.contributor.affiliationLi, Tanda, Univeristy of Sydneyen_AU
local.contributor.affiliationSmalley, B., Keele Universityen_AU
local.contributor.affiliationStello, Dennis, University of Sydneyen_AU
local.contributor.affiliationWhite, Timothy, College of Science, ANUen_AU
local.contributor.affiliationBall, Warrick, University of Birminghamen_AU
local.contributor.affiliationChaplin, W. J., Aarhus Universityen_AU
local.contributor.affiliationColman, Isabel L., University of Sydneyen_AU
local.contributor.affiliationIreland, Michael, College of Science, ANUen_AU
local.contributor.affiliationRains, Adam, College of Science, ANUen_AU
local.contributor.authoruidWhite, Timothy, u1073028en_AU
local.contributor.authoruidIreland, Michael, u5544212en_AU
local.contributor.authoruidRains, Adam, u5841414en_AU
local.description.embargo2099-12-31
local.description.notesImported from ARIESen_AU
local.identifier.absfor370609 - Seismology and seismic explorationen_AU
local.identifier.absfor510109 - Stellar astronomy and planetary systemsen_AU
local.identifier.ariespublicationa383154xPUB13617en_AU
local.identifier.citationvolume581en_AU
local.identifier.doi10.1038/s41586-020-2226-8en_AU
local.identifier.scopusID2-s2.0-85084627221
local.publisher.urlhttps://www.nature.com/en_AU
local.type.statusPublished Versionen_AU

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