Book contents
- Frontmatter
- Contents
- Preface
- 1 A selective overview
- I Stellar convection and oscillations
- II Stellar rotation and magnetic fields
- III Physics and structure of stellar interiors
- IV Helio- and asteroseismology
- 16 Solar structure and the neutrino problem
- 17 Helioseismic data analysis
- 18 Seismology of solar rotation
- 19 Telechronohelioseismology
- V Large-scale numerical experiments
- VI Dynamics
17 - Helioseismic data analysis
Published online by Cambridge University Press: 11 November 2009
- Frontmatter
- Contents
- Preface
- 1 A selective overview
- I Stellar convection and oscillations
- II Stellar rotation and magnetic fields
- III Physics and structure of stellar interiors
- IV Helio- and asteroseismology
- 16 Solar structure and the neutrino problem
- 17 Helioseismic data analysis
- 18 Seismology of solar rotation
- 19 Telechronohelioseismology
- V Large-scale numerical experiments
- VI Dynamics
Summary
The last decade has seen an impressive improvement in the quality and quantity of helioseismic data. While much of the progress has come from a new generation of instruments, such as GONG and MDI, data analysis has also played a major role. In this review I will start with a brief discussion of how the basic analysis of helioseismic data is done. I will then discuss some of the data analysis problems, their influence on our inferences about the Sun and speculate on what improvements may be expected in the near future. Finally I will show a selection of recent results.
Introduction
Until recently most research in helioseismology has used modes in the low (l ≤ 3) and medium (3 < l ≤ 200) degree (l) ranges. Here I will concentrate on the methods and problems in the study of medium-degree modes as well as show selected results. Most studies of modes of high degree (l > 200) have used entirely different analysis methods, such as time-distance analysis, which is discussed elsewhere in this volume (Kosovichev 2003). However, I will touch on some of the issues regarding the analysis of the high-degree modes by methods similar to those used for the medium-degree modes. The reader is also referred to Haber et al. (2002) for results from a technique known as ring diagrams which also uses high-degree modes.
I will start by providing some background material on solar oscillations in Section 17.2.
- Type
- Chapter
- Information
- Stellar Astrophysical Fluid Dynamics , pp. 247 - 262Publisher: Cambridge University PressPrint publication year: 2003
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