© 1990

Solar Photosphere: Structure, Convection, and Magnetic Fields

Proceedings of the 138th Symposium of the International Astronomical Union, Held in Kiev, U.S.S.R., May 15–20, 1989

  • J. O. Stenflo
Conference proceedings

Part of the International Astronomical Union book series (IAUS, volume 138)

Table of contents

  1. Front Matter
    Pages i-xii
  2. Global Properties of the Photosphere

    1. Front Matter
      Pages 1-1
    2. Eugene H. Avrett
      Pages 3-22
    3. N. G. Shchukina, T. G. Shcherbina, R. J. Rutten
      Pages 29-34
    4. E. A. Gurtovenko, R. I. Kostik, R. J. Rutten
      Pages 35-40
  3. Photospheric Fine Structure

    1. Front Matter
      Pages 47-47
    2. A. M. Title, R. A. Shine, T. D. Tarbell, K. P. Topka, G. B. Scharmer
      Pages 49-66
    3. V. N. Karpinsky
      Pages 67-79
    4. Z. Suemoto, E. Hiei
      Pages 97-100
  4. Small-scale Magnetic Fields

    1. Front Matter
      Pages 101-101
    2. S. K. Solanki
      Pages 103-120
    3. T. Tarbell, S. Ferguson, Z. Frank, R. Shine, A. Title, K. Topka et al.
      Pages 147-152
    4. H. C. Dara, C. E. Alissandrakis, S. Koutchmy
      Pages 153-156

About these proceedings


Solar and stellar photospheres constitute the layers most accessible to observations, forming the interface between the interior and the outside of the stars. The solar atmosphere is a rich physics laboratory, in which the whole spectrum of radiative, dynamical, and magnetic processes that tranfer energy into space can be observed. As the fundamental processes take place on very small spatial scales, we need high· resolution observations to explore them. On the other hand the small-scale processes act together to form global properties of the sun, which have their origins in the solar interior. The rapid advances in observational techniques and theoreticallllodelling over the past decade made it very timely to bring together scientists from east and west to the first lAU Symposium on this topic. The physics of the photosphere involves complicated interactions between magnetic fields, convection, waves, and radiation. During the past decade our understanding of these gener­ ally small-scale structures and processes has been dramatically advanced. New instrumen­ tations, on ground and in space, have given us new means to study the granular convection. Diagnostic methods in Stokes polarimetry have allowed us to go beyond the limitations of spatial resolution to explore the structure and dynamics of the subarcsec magnetic struc­ tures. Extensive numerical simulations of the interaction between convection and magnetic fields using powerful supercomputers are providing deepened physical insight. Granulation, magnetic fields, and dynamo processes are being explored in the photospheres of other stars, guided by our improved understanding of the solar photosphere.


Main sequence Photosphere Sunspot helioseismology solar

Editors and affiliations

  • J. O. Stenflo
    • 1
  1. 1.Institute of AstronomyZurichSwitzerland

Bibliographic information

  • Book Title Solar Photosphere: Structure, Convection, and Magnetic Fields
  • Book Subtitle Proceedings of the 138th Symposium of the International Astronomical Union, Held in Kiev, U.S.S.R., May 15–20, 1989
  • Editors Jan Olof Stenflo
  • Series Title International Astronomical Union
  • DOI
  • Copyright Information Springer Science+Business Media B.V. 1990
  • Publisher Name Springer, Dordrecht
  • eBook Packages Springer Book Archive
  • Hardcover ISBN 978-0-7923-0529-3
  • Softcover ISBN 978-0-7923-0530-9
  • eBook ISBN 978-94-009-1061-4
  • Edition Number 1
  • Number of Pages XII, 560
  • Number of Illustrations 0 b/w illustrations, 0 illustrations in colour
  • Topics Astrophysics and Astroparticles
  • Buy this book on publisher's site