Hostname: page-component-84b7d79bbc-7nlkj Total loading time: 0 Render date: 2024-07-26T18:33:55.479Z Has data issue: false hasContentIssue false
  • English
  • Français

Non-Radial Oscillations in Red Giants

Published online by Cambridge University Press:  30 March 2016

Douglas Keeley
Douglas Keeley*
Affiliation:
Science Applications, Inc., Palo Alto, California, U.S.A.

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.

The structure of red giant stars allows non-radial oscillation modes which propagate as p-modes near the surface, to propagate below the convection zone as g-modes with very high radial wave number [Dziembowski (1971, 1977), Shibahashi and Osaki (1976)]. Under some conditions the oscillations in these two propagation regions can be treated as virtually independent normal modes [Shibahashi and Osaki (1976)]. This paper examines the situation in which this approximation is not good, and discusses possible observational consequences of the interaction of the two propagation regions.

The linearized differential equations describing non-radial adiabatic oscillations in stars can be written in the form, 1a1b

Type
Joint Discussion
Information
Highlights of Astronomy , Volume 5: Highlights of Astronomy. As presented at the XVIIth General Assembly of the IAU, 1979 , 1980 , pp. 497 - 500
Copyright
Copyright © Cambridge University Press 1980

References

Ando, Hl, and Osaki, Y. 1975. Publ.Astron.Soc.Japan, 27, 581 Google Scholar
Christy, R.F., 1966. Ap. J., 144, 108.Google Scholar
Dziembowski, W., 1971. Acta Astron., 21, 289.Google Scholar
Dziembowski, W., 1977. Acta Astron, 27, 95.Google Scholar
Osaki, Y., 1977. Publ. Astron. Soc. Japan, 29, 235.Google Scholar
Shibahashi, H., and Osaki, Y., 1976. Publ.Astron.Soc.Japan, 28, 199.Google Scholar