ASTEROSEISMOLOGY OF THE SOLAR ANALOGS 16 Cyg A AND B FROM KEPLER OBSERVATIONS
- High Altitude Observatory, NCAR, P.O. Box 3000, Boulder, CO 80307 (United States)
- Kavli Institute for Theoretical Physics, Kohn Hall, University of California, Santa Barbara, CA 93106 (United States)
- Institut d'Astrophysique Spatiale, Univ Paris-Sud, UMR8617, CNRS, Batiment 121, 91405 Orsay Cedex (France)
- Centro de Astrofisica and Faculdade de Ciencias, Universidade do Porto, Rua das Estrelas, 4150-762 Porto (Portugal)
- Laboratoire Lagrange, UMR7293, Observatoire de la Cote d'Azur, Universite de Nice Sophia-Antipolis, CNRS, BP 4229, 06304 Nice Cedex 4 (France)
- Observatoire de Geneve, Universite de Geneve, 51 Ch. des Maillettes, CH-1290 Sauverny (Switzerland)
- Department of Physics and Astronomy, Aarhus University, DK-8000 Aarhus C (Denmark)
- Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006 (Australia)
- Department of Astronomy and Space Sciences, Ege University, Bornova, 35100 Izmir (Turkey)
- Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005 (India)
- School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT (United Kingdom)
- Instituto de Astrofisica de Canarias, 38205 La Laguna, Tenerife (Spain)
The evolved solar-type stars 16 Cyg A and B have long been studied as solar analogs, yielding a glimpse into the future of our own Sun. The orbital period of the binary system is too long to provide meaningful dynamical constraints on the stellar properties, but asteroseismology can help because the stars are among the brightest in the Kepler field. We present an analysis of three months of nearly uninterrupted photometry of 16 Cyg A and B from the Kepler space telescope. We extract a total of 46 and 41 oscillation frequencies for the two components, respectively, including a clear detection of octupole (l = 3) modes in both stars. We derive the properties of each star independently using the Asteroseismic Modeling Portal, fitting the individual oscillation frequencies and other observational constraints simultaneously. We evaluate the systematic uncertainties from an ensemble of results generated by a variety of stellar evolution codes and fitting methods. The optimal models derived by fitting each component individually yield a common age (t = 6.8 {+-} 0.4 Gyr) and initial composition (Z{sub i} = 0.024 {+-} 0.002, Y{sub i} = 0.25 {+-} 0.01) within the uncertainties, as expected for the components of a binary system, bolstering our confidence in the reliability of asteroseismic techniques. The longer data sets that will ultimately become available will allow future studies of differential rotation, convection zone depths, and long-term changes due to stellar activity cycles.
- OSTI ID:
- 22047966
- Journal Information:
- Astrophysical Journal Letters, Vol. 748, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 2041-8205
- Country of Publication:
- United States
- Language:
- English
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