Hostname: page-component-745bb68f8f-mzp66 Total loading time: 0 Render date: 2025-01-13T10:59:37.259Z Has data issue: false hasContentIssue false
  • English
  • Français

Solar Models with Low Opacity*

Published online by Cambridge University Press:  12 April 2016

P.A. Kuzurman  and
A.A. Pamyatnykh
P.A. Kuzurman
Affiliation:
Astronomical Council of the Academy of Sciences of the USSR
A.A. Pamyatnykh
Affiliation:
Astronomical Council of the Academy of Sciences of the USSR

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.

Evolutionary models of the present Sun with standard and artifically low opacity of stellar matter are obtained and adiabatic nonradial oscillations of the models are computed. The opacity x in nonstandard model (which is the first in a series of future models with low χ) was taken half as much as the Cox-Stewart opacity. The central temperature in such model is approximately 10% below the ‘standard’ values, which can explain the neutrino experiment results. Unlike solar models with very low heavy element abundance, the low χ model has approximately standard mass concentration and distribution of the matter in the outer layers – specifically, the standard characteristics of the convection zone. Hence, the spectrum of adiabatic oscillations is similar to that of the standard models and has the same capabilities for the explanation of the observed pulsations.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 66: Problems of Solar and Stellar Oscillations , 1983 , pp. 223 - 230
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

Bahcall, J.N., Huebner, W.F., Magee, N.H. Jr., Merts, A.L., and Ulrich, R.K.: 1973, Astrophys. J. 184, 1.Google Scholar
Christensen-Dalsgaard, J. and Gough, D.O.: 1980, Nature 288, 544.Google Scholar
Christensen-Dalsgaard, J., Gough, D.O., and Morgan, J.G.: 1979, Astron. Astrophys. 73, 121.Google Scholar
Davis, R.J. and Evans, J.C. Jr.: 1978, in Eddy, J.A. (ed.), New Solar Physics, Westview Press, Boulder, Colorado, p. 35.Google Scholar
Dziembowski, W.: 1977, Acta Astron. 27, (2), p. 95.Google Scholar
Dziembowski, W. and Pamyatnykh, A.A.: 1978, in Rösch, J. (ed.), Pleins feux sur la physique solaire, CNRS, Paris, p. 135.Google Scholar
Ergma, E. and Pamyatnykh, A.A.: 1971, Nauchnye Informatsii 20, 71.Google Scholar
Fowler, W.A., Caughlan, G.R., and Zimmerman, B.A.: 1975, Ann. Rev. Astron. Astrophys. 13, 69.Google Scholar
Fricke, K., Stobie, R.S., and Strittmatter, P.A.: 1971, Monthly Notices Roy. Astron. Soc. 154, 23.Google Scholar
Grec, G., Fossat, E., and Pomerantz, M.: 1980, Nature 288, 541.Google Scholar
Herbig, G.H.: 1965, Astrophys. J. 141, 588.Google Scholar
Iben, I. Jr.: 1969, Ann. Phys. 54, 164.Google Scholar
Iben, I. Jr. and Mahaffy, J.: 1976, Astrophys. J. 209, L39.Google Scholar
Newman, M.J. and Fowler, W.A.: 1976, Astrophys. J. 207, 601.Google Scholar
Opher, R.: 1981, Astron. Astrophys. 98, 39.Google Scholar
Peak, L.S.: 1980, Australian J. Phys. 33, 821.Google Scholar
Press, W.H.: 1980, Preprint No. 1313 of Center for Astrophys., Cambridge, Mass.Google Scholar
Rhodes, E.J. Jr., Ulrich, R.K., and Simon, G.W.: 1977, Astrophys. J. 218, 901.Google Scholar
Scuflaire, R., Gabriel, M., and Noels, A.: 1981, Astron. Astrophys. 99, 39.Google Scholar
Shibahashi, H. and Osaki, Y.: 1983, Solar Phys. 82, 231 (this volume).Google Scholar