The Solar Spectrum

Proceedings of the Symposium held at the University of Utrecht 26–31 August 1963

  • Editors
  • C. De Jager
Conference proceedings

Part of the Astrophysics and Space Science Library book series (ASSL, volume 1)

Table of contents

  1. Front Matter
    Pages I-XIV
  2. Opening Address

    1. A. Unsöld
      Pages 1-2
  3. Fourty Years of Solar Spectroscopy

    1. M. Minnaert
      Pages 3-25
  4. The Photosphere

    1. Front Matter
      Pages 27-27
    2. Jean-Claude Pecker
      Pages 29-88
    3. A. Unsöld, Wasaburo Unno, Yasumasa Yamashita
      Pages 102-109
    4. A. Unsöld, F. Roddier
      Pages 110-115
    5. A. Unsöld, J. Evans, R. Michard, R. Servajean
      Pages 116-127
  5. The Quiet Chromosphere

    1. Front Matter
      Pages 129-129
    2. John T. Jefferies
      Pages 131-150
    3. R. Grant Athay
      Pages 151-178
    4. H. E. Hinteregger
      Pages 179-205
    5. R. O. Redman, L. De Feiter
      Pages 206-218
  6. The Active Photosphere and Chromosphere; Spots, Plages, Flares and Prominences

    1. Front Matter
      Pages 219-219
    2. A. Severny
      Pages 221-239
    3. K. O. Kiepenheuer
      Pages 240-248
    4. J. Evans, M. Rigutti, W. De Graaff
      Pages 249-270
  7. The Corona

    1. Front Matter
      Pages 271-271
    2. M. J. Seaton
      Pages 273-279
    3. Donald E. Billings
      Pages 280-292
    4. R. Lüst, D. J. Faulkner, M. De Groot
      Pages 293-310
  8. Particle and Radio Emmission from the Sun

    1. Front Matter
      Pages 311-311
    2. E. Schatzman
      Pages 313-341
    3. A. Maxwell
      Pages 342-397
    4. M. Minnaert, A. Fokker, L. Biermann
      Pages 413-417

About these proceedings


A good deal of our information on solar physics and on solar phenomena is derived from the solar spectrum. A quantitative interpretation of this spectrum was only possible after 1920, after the establishment of Bohr's atomic model, the discovery of Saha's law, and the development of spectrophotometry. The resolving and light gathering powers of our instruments have greatly increased since. We have seen an enormous progress in our theoretical under­ standing of basic atomic phenomena, and of the intricate problems concerned with the transfer of energy through a complicated structure like the sun's outer layers. In particular the observable part of the solar spectrum tremen­ dously enlarged since the introduction, in the years after 1945, of radio­ astronomy, enabling us to study the solar spectrum between wavelengths of some mm to about 15 m, of space research, giving access to the whole electro­ magnetic spectrum below 3000 A, down to about 0. 01 A. Further, the low and high energetic components of the solar particles spectrum have been dis­ covered with space probes (the solar wind), rockets, balloons (the so-called sub­ cosmic-ray particles) and cosmic ray monitors (solar cosmic ray bursts). The extreme wealth of this spectrum, much vaster in extent than the earlier investigators could only dream of, is an important source of information. It looked appropriate to us, after the rapid development of this branch of science,' to invite the world's leading solar physicists to Utrecht for a summa­ rizing symposium on the whole solar spectrum.


astronomy chromosphere cosmic ray solar activity solar physics solar wind

Bibliographic information

  • DOI
  • Copyright Information Springer Science+Business Media B.V. 1965
  • Publisher Name Springer, Dordrecht
  • eBook Packages Springer Book Archive
  • Print ISBN 978-94-010-3589-7
  • Online ISBN 978-94-010-3587-3
  • Series Print ISSN 0067-0057
  • Buy this book on publisher's site