© 1998

Solar Composition and its Evolution — from Core to Corona

Proceedings of an ISSI Workshop 26–30 January 1998, Bern, Switzerland

  • C. Fröhlich
  • M. C. E. Huber
  • S. K. Solanki
  • R. Von Steiger
Conference proceedings

Part of the Space Sciences Series of ISSI book series (SSSI, volume 5)

Table of contents

  1. Front Matter
    Pages i-xii
  2. Unveiling the Secrets of the Sun

    1. R. M. Bonnet
      Pages 1-16
  3. Solar Interior

    1. Front Matter
      Pages 17-17
    2. Jørgen Christensen-Dalsgaard
      Pages 19-36
    3. W. A. Dziembowski
      Pages 37-48
    4. Werner Däppen
      Pages 49-60
    5. Forrest J. Rogers, Carlos A. Iglesias
      Pages 61-70
    6. Sylvie Vauclair
      Pages 71-78
    7. Jean-Paul Zahn
      Pages 79-90
    8. Y. Suzuki
      Pages 91-104
    9. T. BlÖcker, H. Holweger, B. Freytag, F. Herwig, H.-G. Ludwig, M. Steffen
      Pages 105-112
    10. J. Provost, G. Berthomieu, P. Morel
      Pages 117-124
    11. Sylvaine Turck-Chieze
      Pages 125-132
    12. S. Turcotte, J. Christensen-Dalsgaard
      Pages 133-140
    13. Douglas Gough
      Pages 141-158
  4. Lower Solar Atmosphere

    1. Front Matter
      Pages 159-159
    2. N. Grevesse, A. J. Sauval
      Pages 161-174
    3. Sami K. Solanki
      Pages 175-186
    4. P. G. Judge, H. Peter
      Pages 187-202

About these proceedings


The discovery of chemical elements in celestial bodies and the first estimates of the chemical composition of the solar atmosphere were early results of Astrophysics - the subdiscipline of Astronomy that was originally concerned with the general laws of radiation and with spectroscopy. Following the initial quantitative abundance studies by Henry Norris Russell and by Cecilia Payne-Gaposchkin, a tremendous amount of theoretical, observa­ tional, laboratory and computational work led to a steadily improving body of knowledge of photospheric abundances - a body of knowledge that served to guide the theory of stellar evolution. Solar abundances determined from photospheric spectra, together with the very similar abundances determined from carbonaceous chondrites (where extensive information on isotopic composition is available as well), are nowadays the reference for all cosmic composition measures. Early astrophysical studies of the solar photospheric composition made use of atmosphere models and atomic data. Consistent abundances derived from different atmospheric layers and from lines of different strength helped to confirm and estab­ lish both models and atomic data, and eventually led to the now accepted, so-called "absolute" abundance values - which, for practical reasons, however, are usually given relative to the number of hydrogen nuclei.


Variation solar wind star stellar sun

Editors and affiliations

  • C. Fröhlich
    • 1
  • M. C. E. Huber
    • 2
  • S. K. Solanki
    • 3
  • R. Von Steiger
    • 4
  1. 1.Physikalisch-meteorologisches ObservatoriumWorld Radiation CenterDavosSwitzerland
  2. 2.Space Science Department of ESAESTECNoordwijkThe Netherlands
  3. 3.Institute of AstronomyETHZürichSwitzerland
  4. 4.International Space Science InstituteBernSwitzerland

Bibliographic information

  • Book Title Solar Composition and its Evolution — from Core to Corona
  • Book Subtitle Proceedings of an ISSI Workshop 26–30 January 1998, Bern, Switzerland
  • Editors Claus Fröhlich
    M. Huber
    S.K. Solanki
    Rudolf von Steiger
  • Series Title Space Sciences Series of ISSI
  • DOI
  • Copyright Information Kluwer Academic Publishers 1998
  • Publisher Name Springer, Dordrecht
  • eBook Packages Springer Book Archive
  • Hardcover ISBN 978-0-7923-5496-3
  • Softcover ISBN 978-94-010-6022-6
  • eBook ISBN 978-94-011-4820-7
  • Series ISSN 1385-7525
  • Edition Number 1
  • Number of Pages XII, 431
  • Number of Illustrations 0 b/w illustrations, 0 illustrations in colour
  • Topics Astronomy, Observations and Techniques
    Astrophysics and Astroparticles
  • Buy this book on publisher's site
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