Advances in Helio- and Asteroseismology

1. Front Matter

   Pages i-xxi

   PDF

2. Introduction

   1. Front Matter

      Pages 1-1

      PDF

   2. An Overview Of Helio- and Asteroseismology

      • Jørgen Christensen-Dalsgaard

      Pages 3-19

3. Observations of Solar Oscillations

   1. Front Matter

      Pages 19-19

      PDF

   2. Helioseismology from the South Pole The 1984/85 campaign

      • B. Gelly, E. Fossat, G. Grec, M. Pomerantz

      Pages 21-23

   3. Splitting of the Low ℓ Solar p Modes

      • S. M. Jefferies, C. P. McLeod, H. B. van der Raay, P. L. Palle, T. Roca Cortés

      Pages 25-28

   4. Helioseismic Observations at Stanford, 1977–1986

      • Harald M. Henning, Philip H. Scherrer

      Pages 29-32

   5. Observations of Solar Global Oscillations (1983–1985) And Potential Influence of Terrestrial Sources of Errors

      • A. B. Severny, V. A. Kotov, T. T. Tsap

      Pages 33-36

   6. Intermediate Degree Solar Oscillations

      • T. L. Duvall Jr., J. W. Harvey, M. A. Pomerantz

      Pages 37-40

   7. Measurements of Solar Internal Rotation Obtained with the Mt. Wilson 60-Foot Solar Tower

      • Edward J. Rhodes Jr., Alessandro Cacciani, Martin Woodard, Steven Tomczyk, Sylvain Korzennik, Roger K. Ulrich

      Pages 41-44

   8. Solar Equatorial Rotation Rate Inferred From Inversion of Frequency Splitting of High-Degree Modes

      • Frank Hill, Douglas Gough, Juri Toomre, Deborah A. Haber

      Pages 45-48

   9. Rotation in the Solar Convection Zone Inferred from Fabry-Perot Observations of the 5-Min Oscillations

      • Frank Hill, David M. Rust, Thierry Appourchaux

      Pages 49-52

   10. Comparison of Solar Oscillation Data Obtained from a Study of the Na and K Fraunhoffer Absorption Lines

       • G. R. Isaak, C. P. McLeod, H. B. van der Raay, P. L. Palle, T. Roca Cortes

       Pages 53-57

   11. Response of the Solar Five-Minute Oscillations to a Major Flare

       • Deborah A. Haber, Juri Toomre, Frank Hill

       Pages 59-62

   12. Solar 5-min Oscillation Amplitude Anisotropy and Doppler Velocity Systematics

       • J. R. Kuhn, C. M. O’Neill, L. B. Gilliam

       Pages 63-65

   13. Ground Based Observations of Solar Luminosity Oscillations

       • B. N. Andersen, V. Domingo

       Pages 67-69

   14. Earth Based Observations of Solar Luminosity Oscillations

       • A. Jiménez, P. L. Pallé, F. Pérez Hernández, C. Régulo, T. Roca Cortés, V. Domingo et al.

       Pages 71-74

   15. On the 160 Minute Oscillation

       • P. L. Pallé, T. Roca Cortés

       Pages 75-78

   16. Search For Solar G-Modes from 1981 to 1985

       • P. L. Pallé, T. Roca Cortés

       Pages 79-82

   17. Solar Gravity Modes from Acrim/Smm Irradiance Data

       • Claus Fröhlich

       Pages 83-86

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.

• Main sequence
• Photosphere
• Planet
• Solar
• Sun
• Sunspot
• asteroseismology
• astrophysics
• helioseismology

• Institute of Astronomy, University of Aarhus, Aarhus, Denmark

  Jørgen Christensen-Dalsgaard, Søren Frandsen

Policies and ethics