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

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From: Nature(Vol. 581, Issue 7807)
Publisher: Nature Publishing Group
Document Type: Report
Length: 9,885 words
Lexile Measure: 1510L

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Author(s): Timothy R. Bedding 1 2 , Simon J. Murphy 1 2 , Daniel R. Hey 1 2 , Daniel Huber 3 , Tanda Li 1 2 4 , Barry Smalley 5 , Dennis Stello 2 6 , Timothy R. White 1 2 7 , Warrick H. Ball 2 4 , William J. Chaplin 2 4 , Isabel L. Colman 1 2 , Jim Fuller 8 , Eric Gaidos 9 , Daniel R. Harbeck 10 , J. J. Hermes 11 , Daniel L. Holdsworth 12 , Gang Li 1 2 , Yaguang Li 1 2 13 , Andrew W. Mann 14 , Daniel R. Reese 15 , Sanjay Sekaran 16 , Jie Yu 17 , Victoria Antoci 2 18 , Christoph Bergmann 6 , Timothy M. Brown 10 , Andrew W. Howard 8 , Michael J. Ireland 7 , Howard Isaacson 19 , Jon M. Jenkins 20 , Hans Kjeldsen 2 21 , Curtis McCully 10 , Markus Rabus 10 22 , Adam D. Rains 7 , George R. Ricker 23 24 , Christopher G. Tinney 6 , Roland K. Vanderspek 23 24

Author Affiliations:

(1) Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Camperdown, Australia

(2) Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Aarhus, Denmark

(3) Institute for Astronomy, University of Hawai'i, Honolulu, USA

(4) School of Physics and Astronomy, University of Birmingham, Birmingham, UK

(5) Astrophysics Group, Lennard-Jones Laboratories, Keele University, Keele, UK

(6) School of Physics, University of New South Wales, Kensington, Australia

(7) Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University, Canberra, Australia

(8) TAPIR, California Institute of Technology, Pasadena, USA

(9) Department of Earth Sciences, University of Hawai'i, Honolulu, USA

(10) Las Cumbres Observatory Global Telescope, Goleta, USA

(11) Department of Astronomy, Boston University, Boston, USA

(12) Jeremiah Horrocks Institute, University of Central Lancashire, Preston, UK

(13) Department of Astronomy, Beijing Normal University, Beijing, China

(14) Department of Physics and Astronomy, University of North Carolina at Chapel Hill, Chapel Hill, USA

(15) LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, Meudon, France

(16) Instituut voor Sterrenkunde (IvS), KU Leuven, Leuven, Belgium

(17) Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany

(18) DTU Space, National Space Institute, Technical University of Denmark, Kongens Lyngby, Denmark

(19) Department of Astronomy, University of California at Berkeley, Berkeley, USA

(20) NASA Ames Research Center, Moffett Field, USA

(21) Institute of Theoretical Physics and Astronomy, Vilnius University, Vilnius, Lithuania

(22) Department of Physics, University of California, Santa Barbara, USA

(23) Department of Physics, Massachusetts Institute of Technology, Cambridge, USA

(24) Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, USA

Main

The [delta] Scuti variables are stars of intermediate mass (1.5-2.5 solar masses, M â ) that pulsate in low-order pressure modes6,7 . Observations have shown that many [delta] Scuti stars have regular frequency spacings in their pulsation spectra (see Methods) but a large sample with unambiguous mode identifications is lacking. Each pulsation mode in a non-rotating star is identified by two integers: the radial order, n , and the degree, l . We expect the strongest observable modes to be of low degree (l = 0, 1 and 2), because higher degrees have greatly reduced amplitudes due to cancellation in disk-integrated light. In the so-called asymptotic regime ( n [much greater-than] l ), modes with a given degree l are approximately equally spaced in frequency by a...

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Gale Document Number: GALE|A623825876