Hostname: page-component-78c5997874-8bhkd Total loading time: 0 Render date: 2024-11-09T13:30:49.375Z Has data issue: false hasContentIssue false
  • English
  • Français

Stellar Seismology

Published online by Cambridge University Press:  12 April 2016

Werner Däppen
Werner Däppen*
Affiliation:
Space Science Department of ESA, ESTEC, 2200 AG Noordwijk, The Netherlands

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.

Stellar acoustic oscillation frequencies will likely be accurately observed in the near future, in analogy to the well-known solar five-minute oscillation frequencies. Of course, we will never expect the wealth of solar data, which is a result of spatial resolution. We will therefore not be able to solve the inverse problem, that is to probe physical quantities as functions of depth, and the low number of anticipated observed frequencies will make an unambiguous mode identification difficult. Despite this restriction to the forward problem, however, observed stellar oscillation frequencies will become valuable constraints for the determination of stellar parameters. One should not forget that the present knowledge of stellar ages and compositions relies on the calibration of theoretical models (matching effective temperature and luminosity). Additional observational constraints will improve these calibrations, even if the theoretical models themselves are not questioned. We hope, however, that the observation of stellar oscillation frequencies will also lead to improvements in the physics of stellar models, in analogy to the solar case. Again, of course, stellar seismologists will be less ambitious than helioseismologists, since there are more open parameters in stellar models. However, stellar observations will allow tests of models with different age and composition.

Type
Part 3: Helioseismology
Information
International Astronomical Union Colloquium , Volume 121: Inside the Sun , 1990 , pp. 357 - 370
Copyright
Copyright © Kluwer 1990

References

Baade, D. 1988a, in The Impact of Very High S/N Spectroscopy on Stellar Physics, eds. Cayrel de Strobel, G. & Spite, M. (IAU Symp. 132, Kluwer, Dordrecht), 193–198.Google Scholar
Baade, D. 1988b, in The Impact of Very High S/N Spectroscopy on Stellar Physics, eds. Cayrel de Strobel, G. & Spite, M. (IAU Symp. 132, Kluwer, Dordrecht), 217–222.Google Scholar
Christensen-Dalsgaard, J. 1984, in Proc. workshop on space research prospects in stellar activity and variability, eds. Mangeney, A. & Praderie, P. (Paris Observatory Press), 11–45.Google Scholar
Christensen-Dalsgaard, J. 1986, in Seismology of the Sun and the Distant Stars, ed. Gough, D.O. (NATO ASI Series, Reidel, Dordrecht), 3–18.Google Scholar
Christensen-Dalsgaard, J. 1988, in Advances in Helio- and Asteroseismology, eds. Christensen-Dalsgaard, J. and Frandsen, S. (IAU Symp. 123, Reidel, Dordrecht), 3–18.Google Scholar
Christensen-Dalsgaard, J., Berthomieu, G. 1990, in Solar Interior and Atmosphere, eds. Cox, A. N., Livingston, W. C., & Matthews, M. ( Space Science Series, University of Arizona Press), in press.Google Scholar
Cox, A.N., Chitre, S.M., Frandsen, S., Kumar, P. 1990, in Solar Interior and Atmosphere, eds. Cox, A. N., Livingston, W. C., & Matthews, M. ( Space Science Series, Unversity of Arizona Press), in press.Google Scholar
Däppen, W., Dziembowski, W., Sienkiewicz, R. 1988, in Advances in Helio- and Asteroseismology, eds. Christensen-Dalsgaard, J. and Frandsen, S. (IAU Symp. 123, Reidel, Dordrecht), 233–247.Google Scholar
Deubner, F.-L., Gough, D.O. 1984, Ann. Rev. Astron. Astrophys., 22, 593–619.Google Scholar
Gabriel, M. 1990, The l-dependent part of Dnl and the structure of the solar core, Solar Physics, (submitted).Google Scholar
Gelly, B., Grec, G., Fossat, E. 1986, Astron. Astrophys., 164, 383–394.Google Scholar
Gough, D.O. 1985, in Future Missions in Solar, Heliospheric, and Space Plasma Physics, ed. Rolfe, E., ESA SP-235, European Space Agency, Noordwijk), 183–197.Google Scholar
Gough, D.O. 1987, Nature, 326, 257–259.Google Scholar
Guenther, D.B., Demarque, P. 1985, Astrophys. J., 301, 207.Google Scholar
Lamb, H. 1932, Hydrodynamic, (Cambridge Univ. Press, Cambridge).Google Scholar
Noyes, R.W., Baliunas, S.L., Belserene, E., Duncan, D.K., Horne, J., Widrow, L. 1984, Astrophys. J. Letters, 285, L23.Google Scholar
Schwarzschild, M. 1958, Structure and Evolution of the Stars, (Princeton Univ. Press, Princeton).CrossRefGoogle Scholar
Smith, M. 1985, Astrophys. J., 297, 206–223.Google Scholar
Soderblom, D., Däppen, W. 1989, Astrophys. J., (in press).Google Scholar
Tassoul, M. 1980, Astrophys. J. Suppl. Ser., 43, 469–490.Google Scholar
Ulrich, R.K. 1988, in Advances in Helio- and Asteroseismology, eds. Christensen-Dalsgaard, J. and Frandsen, S. (IAU Symp. 123, Reidel, Dordrecht), 299–302.Google Scholar
Ulrich, R.K. 1986, Astrophys. J., 306, L37–L40.Google Scholar
Unno, W., Osaki, Y., Ando, H., Shibahashi, H. 1979, Nonradial Oscillations of Stars, (University of Tokyo Press).Google Scholar
van den Bergh, S. 1989, Astron. Astrophys. Rev., 1, 111–139.Google Scholar