Hostname: page-component-7bb8b95d7b-fmk2r Total loading time: 0 Render date: 2024-09-19T04:52:55.897Z Has data issue: false hasContentIssue false

Overview of the conference: implications of seismological data for astrophysics

Published online by Cambridge University Press:  03 August 2017

Arthur N. Cox*
Affiliation:
Theoretical Division, MS B288, Los Alamos National Laboratory, Los Alamos, New Mexico 87545

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.

This review of the conference will necessarily consider the seismological data implications for only stellar astrophysics. While there are some aspects of this conference that interface with subjects like relativity, gravity, stellar systems, studies of chaos, etc., these will not be discussed here. What we are doing here is discussing the interiors of stars. We want to learn about their masses and composition structures. Pulsation periods can be used to measure stellar mean densities. Further details that seem accessible are the solar rotation speed versus depth and latitude and the structure of both solar and stellar atmospheres.

Most of the contributions at this conference dealt with the hard problems of our understanding oscillations of the sun. As we shall see in many cases, the problems in understanding the stars by observing their pulsation periods are even more difficult. Similarities and differences between helioseismology and asteroseismology will be a principal theme of this review.

Type
Chapter 11: Summary of the Conference
Copyright
Copyright © Reidel 1988 

References

Aizenman, M.L., Hansen, C.J., and Ross, R.R. 1975, Ap. J. 201, 387.CrossRefGoogle Scholar
Ando, H. and Osaki, Y. 1975, Pub. Ast. Soc. Japan, 27, 581.Google Scholar
Antia, H. M., Chitre, S.M. and Narasimha, D. 1982, Solar Phys. 77, 303.CrossRefGoogle Scholar
Christensen-Dalsgaard, J. and Frandsen, S. 1983, in Problems of Solar and Stellar Oscillations (Reidel: Dordrecht) p 165.Google Scholar
Christensen-Dalsgaard, J., Gough, D. and Toomre, J. 1985, Science 229, 923.CrossRefGoogle Scholar
Dappen, W., Gilliland, R.L., and Christensen-Dalsgaard, J. 1986, Nature, 321, 229.CrossRefGoogle Scholar
Faulkner, J. and Gilliland, R. L. 1985, Ap. J. 299, 994.Google Scholar
Faulkner, J., Gough, D.O., and Vahia, M.N. 1986, Nature 321, 226.CrossRefGoogle Scholar
Goldreich, P. and Keeley, D.A. 1977a, Ap. J. 211, 934.CrossRefGoogle Scholar
Goldreich, P. and Keeley, D.A. 1977b, Ap. J. 212, 243.Google Scholar
Guenther, D.B. and Demarque, P. 1986, Ap. J. 301, 207.CrossRefGoogle Scholar
Kidman, R.B. and Cox, A. N. 1984, in Solar Seismology from Space, JPL 84-84 p. 335.Google Scholar
Lebreton, Y. and Maeder, A. 1986, Astron. Astrophys. 161, 119.Google Scholar
Saio, H. 1980, Ap. J. 240, 685.Google Scholar
Souffrin, P. and Spiegel, E.A. 1967, Ann. Astrophys. 30, 985.Google Scholar
Spiegel, E.A. 1964, Ap. J. 139, 959.CrossRefGoogle Scholar
Stellingwerf, R.F. 1975a, Ap. J. 195, 441.CrossRefGoogle Scholar
Stellingwerf, R.F. 1975b, Ap. J. 199, 705.CrossRefGoogle Scholar
van der Raay, H.B. 1984, in Theoretical Problems in Stellar Stability and Oscillations (Liege: Universite de Liege) p 215.Google Scholar
Ziebarth, K. 1970, Ap. J. 162, 947.CrossRefGoogle Scholar