The seismic structure of the sun

D. O. Gough, A. G. Kosovichev, J. Toomre, E. Anderson, H. M. Antia, S. Basu, B. Chaboyer, S. M. Chitre, J. Christensen-Dalsgaard, W. A. Dziembowski, A. Eff-Darwich, J. R. Elliott, P. M. Giles, P. R. Goode, J. A. Guzik, J. W. Harvey, F. Hill, J. W. Leibacher, M. J.P.F.G. Monteiro, O. RichardT. Sekii, H. Shibahashi, M. Takata, M. J. Thompson, S. Vauclair, S. V. Vorontsov

Research output: Contribution to journalArticlepeer-review

174 Scopus citations


Global Oscillation Network Group data reveal that the internal structure of the sun can be well represented by a calibrated standard model. However, immediately beneath the convection zone and at the edge of the energy-generating core, the sound-speed variation is somewhat smoother in the sun than it is in the model. This could be a consequence of chemical inhomogeneity that is too severe in the model, perhaps owing to inaccurate modeling of gravitational settling or to neglected macroscopic motion that may be present in the sun. Accurate knowledge of the sun's structure enables inferences to be made about the physics that controls the sun; for example, through the opacity, the equation of state, or wave motion. Those inferences can then be used elsewhere in astrophysics.

Original languageEnglish (US)
Pages (from-to)1296-1300
Number of pages5
Issue number5266
StatePublished - May 31 1996

All Science Journal Classification (ASJC) codes

  • General


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