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The Seismic Structure of the Sun

Gough1, Kosovichev, Toomre

  • 1D. O. Gough, J. R. Elliott, and T. Sekii are with the Institute of Astronomy, University of Cambridge, CB3 0HA, UK. A. G. Kosovichev and P. R. Giles are with HEPL, Stanford University, Stanford, CA, USA. J. Toomre is at JILA, University of Colorado, Boulder, CO, USA. E. Anderson, J. W. Harvey, F. Hill, and J. W. Leibacher are at the National Solar Observatory, Tucson, AZ, USA. H. M. Antia and S. M. Chitre are at the Tata Institute for Fundamental Research, Bombay, India. S. Basu and J. Christensen-Dalsgaard are at the Theoretical Astrophysics Centre, Aarhus University, Denmark. B. Chaboyer is at the Canadian Institute for Theoretical Astrophysics, Toronto, Canada. W. A. Dziembowski is at the Copernicus Astronomical Center, Warsaw, Poland. A. Eff-Darwich is at the Instituto Astrofisico de Canarias, Tenerife, Canary Islands. P. R. Goode is at the New Jersey Institute of Technology, Newark, NJ, USA. J. A. Guzik is at the Los Alamos National Laboratory, Los Alamos, NM, USA. M. J. P. F. G. Monteiro is at the University of Oporto, Postugal. O. Richard and S. Vauclair are at the Observatoire Midi-Pyrenees, Toulouse, France. H. Shibahashi and M. Takata are in the Department of Astronomy, University of Tokyo, Tokyo, Japan. M. J. Thompson and S. V. Vorontsov are at Queen Mary and Westfield College, University of London, London, UK.

Science (New York, N.Y.)
|May 31, 1996
PubMed
Summary

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Helioseismology data show the sun's internal structure aligns with standard models, but with smoother sound-speed variations near the core. This suggests potential inaccuracies in solar models regarding chemical composition or internal motion.

Area of Science:

  • Solar physics
  • Helioseismology
  • Astrophysical modeling

Background:

  • The Sun's internal structure is crucial for understanding stellar physics.
  • Standard solar models are widely used but may have limitations.

Purpose of the Study:

  • To compare the Sun's internal structure with a calibrated standard model using helioseismology data.
  • To identify discrepancies and investigate their potential causes.

Main Methods:

  • Analysis of data from the Global Oscillation Network Group (GONG).
  • Comparison of observed sound-speed variations with predictions from a standard solar model.

Main Results:

  • Helioseismology data generally agree with the standard solar model.

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  • A smoother sound-speed variation was observed in the Sun beneath the convection zone compared to the model.
  • This discrepancy may stem from inaccuracies in modeling gravitational settling or unmodeled macroscopic motions.
  • Conclusions:

    • The findings highlight potential areas for improvement in solar models, specifically concerning chemical inhomogeneity and internal dynamics.
    • Accurate solar structure knowledge aids in understanding fundamental physics (opacity, equation of state, wave motion) applicable across astrophysics.