Overview
- Editors:
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Jørgen Christensen-Dalsgaard
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Institute of Astronomy, University of Aarhus, Aarhus, Denmark
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Søren Frandsen
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Institute of Astronomy, University of Aarhus, Aarhus, Denmark
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Table of contents (110 papers)
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Introduction
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- Jørgen Christensen-Dalsgaard
Pages 3-19
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Observations of Solar Oscillations
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- B. Gelly, E. Fossat, G. Grec, M. Pomerantz
Pages 21-23
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- S. M. Jefferies, C. P. McLeod, H. B. van der Raay, P. L. Palle, T. Roca Cortés
Pages 25-28
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- Harald M. Henning, Philip H. Scherrer
Pages 29-32
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- A. B. Severny, V. A. Kotov, T. T. Tsap
Pages 33-36
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- T. L. Duvall Jr., J. W. Harvey, M. A. Pomerantz
Pages 37-40
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- Edward J. Rhodes Jr., Alessandro Cacciani, Martin Woodard, Steven Tomczyk, Sylvain Korzennik, Roger K. Ulrich
Pages 41-44
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- Frank Hill, Douglas Gough, Juri Toomre, Deborah A. Haber
Pages 45-48
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- Frank Hill, David M. Rust, Thierry Appourchaux
Pages 49-52
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- G. R. Isaak, C. P. McLeod, H. B. van der Raay, P. L. Palle, T. Roca Cortes
Pages 53-57
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- Deborah A. Haber, Juri Toomre, Frank Hill
Pages 59-62
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- J. R. Kuhn, C. M. O’Neill, L. B. Gilliam
Pages 63-65
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- B. N. Andersen, V. Domingo
Pages 67-69
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- A. Jiménez, P. L. Pallé, F. Pérez Hernández, C. Régulo, T. Roca Cortés, V. Domingo et al.
Pages 71-74
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- P. L. Pallé, T. Roca Cortés
Pages 75-78
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- P. L. Pallé, T. Roca Cortés
Pages 79-82
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About this book
Helio- and asteroseismology study the interior of the Sun and other stars, by means of observations of oscillations on their surfaces. The last 10 years in the study of the solar interior, to a has witnessed a very rapid evolution point where we can now contemplate investigating the physical state of matter, or the details of rotation and other large-scale motion, in the Sun. The stellar studies are in some respects at the point of the solar studies 10 years ago, but appear poised to take off. Thus the time was deemed ripe for lAO Symposium No 123, to assess the present status of this work, and plan for its future development. Apart from the seismic data, few observations are available to provide information about stellar interiors. Detailed studies, by spectral analysis, can be made of stellar surface properties, including atmospheric temperature and chemical composition. However, the stellar radiative spectrum is almost entirely fixed by the mass, luminosity, radius and surface rotation of the star, and contains essentially no other information about the interior. An important test of stellar evolution theory is provided by observations of stel lar clusters, whose members can reasonably be assumed to have the same age and chemical composition. The location of such stars in a HR diagram, where luminosity is plotted against the effective temperature, can roughly be understood in terms of stellar evolution calculations.
