Статья

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

T. R. BeddingStellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Aarhus, Denmark. [email protected]Simon J. MurphyStellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Aarhus, DenmarkDaniel HeyStellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Aarhus, DenmarkDaniel HuberInstitute for Astronomy, University of Hawai'i, Honolulu, HI, USATanda LiSchool of Physics and Astronomy, University of Birmingham, Birmingham, UKB. SmalleyAstrophysics Group, Lennard-Jones Laboratories, Keele University, Keele, UKDennis StelloSchool of Physics, University of New South Wales, Kensington, New South Wales, AustraliaTimothy R. WhiteResearch School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University, Canberra, Australian Capital Territory, AustraliaWarrick H. BallSchool of Physics and Astronomy, University of Birmingham, Birmingham, UKW. J. ChaplinSchool of Physics and Astronomy, University of Birmingham, Birmingham, UKIsabel L. ColmanStellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Aarhus, DenmarkJim FullerTAPIR, California Institute of Technology, Pasadena, CA, USAEric GaidosDepartment of Earth Sciences, University of Hawai'i, Honolulu, HI, USADaniel HarbeckLas Cumbres Observatory Global Telescope, Goleta, CA, USAJ. J. HermesDepartment of Astronomy, Boston University, Boston, MA, USADaniel L. HoldsworthJeremiah Horrocks Institute, University of Central Lancashire, Preston, UKGang LiStellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Aarhus, DenmarkYaguang LiDepartment of Astronomy, Beijing Normal University, Beijing, ChinaAndrew W. MannDepartment of Physics and Astronomy, University of North Carolina at Chapel Hill, Chapel Hill, NC, USAD R ReeseUniversité Paris CitéSanjay SekaranInstituut voor Sterrenkunde (IvS), KU Leuven, Leuven, BelgiumJie YuMax-Planck-Institut für Sonnensystemforschung, Göttingen, GermanyVictoria AntociDTU Space, National Space Institute, Technical University of Denmark, Kongens Lyngby, DenmarkChristoph BergmannSchool of Physics, University of New South Wales, Kensington, New South Wales, AustraliaTimothy M. BrownLas Cumbres Observatory Global Telescope, Goleta, CA, USAAndrew W. HowardTAPIR, California Institute of Technology, Pasadena, CA, USAMichael J. IrelandResearch School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University, Canberra, Australian Capital Territory, AustraliaHoward IsaacsonDepartment of Astronomy, University of California at Berkeley, Berkeley, CA, USAJon M. JenkinsNASA Ames Research Center, Moffett Field, CA, USAHans KjeldsenInstitute of Theoretical Physics and Astronomy, Vilnius University, Vilnius, LithuaniaCurtis McCullyLas Cumbres Observatory Global Telescope, Goleta, CA, USAMarkus RabusDepartment of Physics, University of California, Santa Barbara, CA, USAAdam D. RainsResearch School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University, Canberra, Australian Capital Territory, AustraliaGeorge R. RickerDepartment of Physics, Massachusetts Institute of Technology, Cambridge, MA, USAChristopher G. TinneySchool of Physics, University of New South Wales, Kensington, New South Wales, AustraliaRoland K. VanderspekDepartment of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA

2020en

ABI

Аннотация

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. The pulsation spectra of intermediate-mass stars (so-called δ Scuti stars) have been challenging to analyse, but new observations of 60 such stars reveal remarkably regular sequences of high-frequency pulsation modes.

Перевод пока недоступен

Идентификаторы

DOI: 10.1038/s41586-020-2226-8

Цитирования и источники

Цитирований: 4Использованных источников: 0

Показатели — AkademScholar