Hostname: page-component-7479d7b7d-k7p5g Total loading time: 0 Render date: 2024-07-11T02:32:35.840Z Has data issue: false hasContentIssue false
  • English
  • Français

Helioseismic Data Reduction

Published online by Cambridge University Press:  08 February 2017

F. Hill
F. Hill*
Affiliation:
National Optical Astronomy Observatories, National Solar Observatory, PO Box 26732, Tucson, AZ 85726-6732, USA

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Helioseismology seeks to infer the properties of the solar interior using measurements of the global normal mode oscillations as a function of spherical harmonic degree l, azimuthal order m, and radial order n as observed on the solar surface. The frequencies, v0(l, m, n), of the modes are influenced by the physical conditions of the solar plasma through which the p-mode (pressure) waves propagate, while the power, P(l, m, n), and line widths, Γ(l, m, n), provide clues about the excitation and damping of the oscillations. These mode parameters are extracted from observations of the solar surface using a long and complex data reduction procedure. It is thus important to precisely describe the steps in the reduction and to assess the influence of the choices on the resulting inferred physical conditions.

Type
I. Global Structure and Evolution of the Solar and Stellar Interior
Information
Symposium - International Astronomical Union , Volume 185: New Eyes to See Inside the Sun and Stars , 1998 , pp. 13 - 20
Copyright
Copyright © Kluwer 1998 

References

Anderson, E.A., Duvall, T.L. Jr., and Jefferies, S.M.: 1990, Astrophys. J., 364, 699.CrossRefGoogle Scholar
Appourchaux, T., Gizon, L., and Rabello-Soares, M.-C.: 1997, Astron. & Astrophys., submitted.Google Scholar
Baudin, F., and Hill, F.: 1997, Bull. Amer. Astron. Soc., 29, 893.Google Scholar
Harvey, J.W., Hill, F., Komm, R., Leibacher, J.W., Pohl, B., and the GONG Team: 1997, these Proceedings.Google Scholar
Hill, F., Anderson, E.A., Armet, D., Chavez, E., Erdwurm, W., Goodrich, J., Harvey, J.W., Hubbard, R.P., Jefferies, S.M., Kennedy, J.R., Ladd, G., Leibacher, J.W., Pintar, J.A., Pohl, B., Toner, C.G., Toussaint, R., Williams, W.E., and Wing, T.: 1998, Solar Phys., in preparation.Google Scholar
Howe, R., and Thompson, M.J.: 1997, Astron. & Atrophys., submitted.Google Scholar
Jefferies, S.M.: 1997, these Proceedings.Google Scholar
Kennedy, J.R.: 1997, Solar Phys. in press.Google Scholar
Kennedy, J.R., and Williams, W.E.: 1997, Solar Phys., submitted.Google Scholar
Komm, R., Gu, Y., Hill, F., Stark, P., and Fodor, I.: 1997, in Proc. Cool Stars, in press.Google Scholar
Schou, J.: 1992, On the Analysis of Helioseismic Data, , Aarhus University, Appendix 4.Google Scholar
Toner, C.G., and Harvey, J.W.: 1997, in Sounding Solar And Stellar Interiors, Proc. IAU Symp. 181, Ed. Berthomieu, G. and Schmider, F.-X., in press.Google Scholar
Toner, C.G., and Jefferies, S.M.: 1993, Astrophys. J., 415, 852.Google Scholar