Hostname: page-component-cd9895bd7-jkksz Total loading time: 0 Render date: 2024-12-26T03:36:41.232Z Has data issue: false hasContentIssue false
  • English
  • Français

On the Excitation of Oscillations of the Sun (Numerical Models)*

Published online by Cambridge University Press:  12 April 2016

A.G. Kosovichev  and
A.B. Severny
A.G. Kosovichev
Affiliation:
Crimean Astrophysical Observatory, p/o Nauchny, 334413, Crimea, U.S.S.R.
A.B. Severny
Affiliation:
Crimean Astrophysical Observatory, p/o Nauchny, 334413, Crimea, U.S.S.R.

Abstract

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.

Numerical solutions of the general time-dependent gas-dynamical equations in linear adiabatic approximation are given for initial conditions imitating: (a) a central perturbation, (b) a boundary perturbation (in the convective envelope), and (c) a ‘shrinking’ of the Sun as a whole. For a variety of models of the Sun it is found that at the surface the radial component vr of velocity is much greater than the tangential component vt, and that the period T of stationary oscillations does not exceed 131m. The appearance at the surface of a g mode with period 160m is found to be improbable.

With the initial conditions adopted, a propagating wave is produced which is reflected successively from the centre to the periphery and back, producing 5-min oscillations at the surface of the Sun. Expansion of this wave into separate modes leads to a power spectrum qualitatively similar to that observed.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 66: Problems of Solar and Stellar Oscillations , 1983 , pp. 323 - 329
Copyright
Copyright © Reidel 1983

Footnotes

*

Proceedings of the 66th IAU Colloquium: Problems in Solar and Stellar Oscillations, held at the Crimean Astrophysical Observatory, U.S.S.R., 1-5 September, 1981.

References

Christensen-Dalsgaard, J. and Gough, D.O.: 1976, Nature 259, 89.Google Scholar
Christensen-Dalsgaard, J. and Gough, D.O.: 1980, Nature 288, 544.Google Scholar
Christensen-Dalsgaard, J., Düke, F.W.W., and Gough, D.O.: 1974, Monthly Notices Roy. Astron. Soc. 169, 429.CrossRefGoogle Scholar
Claverie, A., Isaak, G.R., McLeod, C.P., van der Raay, H.B., and Roca Cortes, T.: 1979, Nature 282, 591.Google Scholar
Dziembowski, W. and Pamyatnykh, A.A.: 1978, in Rösch, (ed.), Plein feux sur la physique solaire, CNRS, Paris, p. 135.Google Scholar
Grec, G., Fossat, E., and Pomerantz, M.: 1980, Nature 288, 541.Google Scholar
Kosovichev, A.G. and Severny, A.B.: 1981, Astron. Zh. Pisma 7, 34.Google Scholar
Iben, I. and Mahaffy, J.: 1976, Astrophys. J. 209, L39.Google Scholar
Pekeris, C.L.: 1938, Astrophys. J. 88, 189.Google Scholar
Robe, H.: 1968, Ann. Astrophys. 31, 475.Google Scholar
Schatzman, E., Maeder, A., Angrand, F., and Glowinski, R.: 1981, Astron. Astrophys. 96, 1.Google Scholar
Thomson, W.: 1863, Phil. Trans. Roy. Soc. London 153, 583.Google Scholar
Vandakurov, Yu. V.: 1967, Astron. Zh. 44, 786.Google Scholar
Vorontsov, S.V. and Zharkov, V.N.: 1968, Astron. Zh. 55, 84.Google Scholar