Chromospheric Fine Structure

  • R. Grant Athay

Part of the International Astronomical Union/Union Astronomique Internationale book series (IAUS, volume 56)

Table of contents

  1. Front Matter
    Pages VI-VII
  2. The Quiet Chromosphere: Limb Phenomena

    1. Front Matter
      Pages 1-1
    2. R. Michard
      Pages 3-21
    3. Jay M. Pasachoff, Frederick S. Harris, Jacques M. Beckers
      Pages 31-32
  3. The Quiet Chromosphere: Disk Phenomena

    1. Front Matter
      Pages 33-33
    2. R. B. Dunn, J. B. Zirker, J. M. Beckers
      Pages 45-47
    3. Harold Zirin
      Pages 49-50
    4. M. R. Kundu, T. Velusamy, R. H. Becker
      Pages 65-68
  4. The Upper Chromosphere

    1. Front Matter
      Pages 69-69
    2. J. T. Jefferies
      Pages 71-88
    3. U. Grossmann-Doerth
      Pages 93-93
  5. Motion and Excitation in the Chromosphere

  6. The Chromosphere in Active Regions

    1. Front Matter
      Pages 159-159
    2. H. Zirin
      Pages 161-175
    3. David E. Rees
      Pages 177-178
    4. E. Wiehr, G. Stellmacher
      Pages 179-181
    5. F. Q. Orrall, R. J. Speer
      Pages 193-196
    6. Joan Vorpahl
      Pages 197-198
  7. Evolution of Chromospheric Fine Structures

    1. Front Matter
      Pages 199-199
    2. Dale Vrabec
      Pages 201-231
    3. F. Meyer, H. U. Schmidt, N. O. Weiss, P. R. Wilson
      Pages 235-237
  8. Energy Balance, Heat Transfer and Heating Mechanisms in Chromospheric Fine Structures

  9. Back Matter
    Pages 303-310

About this book


The devotion of an IA U symposium entirely to the topic of chromo spheric fine structure at a time when models of the spherically symmetric chromosphere are still evolving constitutes a valid recognition of the growing feeling among solar astron­ omers that the chromosphere cannot be understood independently of its discrete structural features. Network structure, which seemingly borders the photospheric supergranule cells, persists intact throughout the chromosphere and most of the chromosphere-corona transition region. The network is the locus of the bright coarse mottles, and the spicule bushes and is the terminus for one end of the quiet chromo­ spheric fibrils as well. Additionally, it is the locus of most of the magnetic flux of the quiet chromosphere. It is not surprising, therefore, that current studies of the chromosphere tend to center around efforts to better describe the network phenom­ ena and to ascertain the physical properties of the network features. Clearly, the supergranule cells and associated network structures constitute a fundamental and singularly important feature of solar structure in the boundary layers. Just as it is now clear that much of the chromo spheric fine structure is associated with the network bordering supergranule cells, it seems equally clear that structural features are almost universally associated with both fluid flow and magnetic geometry. Indeed, many observers claim that the brightness features faithfully map the mag­ netic lines offorce while still others claim that associated with each class of brightness feature there is a more or less unique fluid flow.


Chromosphere Corona LOPES Sunspot solar sun

Editors and affiliations

  • R. Grant Athay
    • 1
  1. 1.High Altitude Observatory of the National Center for Atmospheric Research (Sponsored by the National Science Foundation)BoulderUSA

Bibliographic information

  • DOI
  • Copyright Information Springer Science+Business Media B.V. 1974
  • Publisher Name Springer, Dordrecht
  • eBook Packages Springer Book Archive
  • Print ISBN 978-90-277-0288-3
  • Online ISBN 978-94-010-2103-6
  • Buy this book on publisher's site