Determining distances using asteroseismic methods

Authors

  • V. Silva Aguirre,

    Corresponding author
    1. Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark
    2. Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1, 85748, Garching bei München, Germany
    • Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark
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  • L. Casagrande,

    1. Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, The Australian National University, ACT 2611, Australia
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  • S. Basu,

    1. Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06520-8101, USA
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  • T. L. Campante,

    1. Centro de Astrofísica and Faculdade de Ciências, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
    2. School of Physics and Astronomy, University of Birmingham, Birmingham, B15 2TT, UK
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  • W. J. Chaplin,

    1. Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark
    2. School of Physics and Astronomy, University of Birmingham, Birmingham, B15 2TT, UK
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  • D. Huber,

    1. NASA Ames Research Center, Moffett Field, CA 94035, USA
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  • A. Miglio,

    1. School of Physics and Astronomy, University of Birmingham, Birmingham, B15 2TT, UK
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  • A. M. Serenelli,

    1. Instituto de Ciencias del Espacio (CSIC-IEEC), Facultad de Ciències, Campus UAB, 08193 Bellaterra, Spain
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  • KASC WG#1


Abstract

Asteroseismology has been extremely successful in determining the properties of stars in different evolutionary stages with a remarkable level of precision. However, to fully exploit its potential, robust methods for estimating stellar parameters are required and independent verification of the results is needed. In this talk, I present a new technique developed to obtain stellar properties by coupling asteroseismic analysis with the infrared flux method. Using two global seismic observables and multi-band photometry, the technique determines masses, radii, effective temperatures, bolometric fluxes, and thus distances for field stars in a self-consistent manner. Applying our method to a sample of solar-like oscillators in the Kepler field that have accurate Hipparcos parallaxes, we find agreement in our distance determinations to better than 5 %. Comparison with measurements of spectroscopic effective temperatures and interferometric radii also validate our results, and show that our technique can be applied to stars evolved beyond the main-sequence phase. (© 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)

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