Hostname: page-component-cd9895bd7-mkpzs Total loading time: 0 Render date: 2024-12-25T16:12:09.187Z Has data issue: false hasContentIssue false

4. Non-stable magneto-hydrodynamical processes in stars

Published online by Cambridge University Press:  18 July 2016

A. J. Kipper*
Affiliation:
Tartu Observatory, Tartu, Estonia, 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.

1. The behaviour of the magnetic field of a star was investigated by Cowling, Lamb and Wrubel on the assumption of the star as a solid body and on the assumption that the field variations caused by the extinction do not create any motions of the stellar matter. The important results obtained make possible the interpretation of magneto-hydrodynamical processes in stars only quite roughly. When motions of stellar matter caused by the electromagnetic forces are taken into account new properties may be revealed and the non-stability of the magneto-hydrodynamical processes in stars established. Entangled magnetic fields are the general expression of non-stability.

2. The mathematical criterion of a confused stellar magnetic field is given in the preceding paper from the magneto-hydrodynamical equations for an ideal incompressible fluid. The conception of a confused field as a superposition of various fields of different scales is introduced.

3. It is known that the presence of a magnetic field causes an increase of the stability of hydrodynamical processes, as compared with processes in the absence of a magnetic field. It may most probably be concluded that the extent of confusion of a magnetic field is not the same, as it happens as a result of ordinary turbulent motions in a liquid. However, owing to magneto-hydrodynamical formulae, it may be stated in the present paper that if the field confusion is considered as a superposition of fields of different dimensions and not as a field of entangled magnetic lines, no stability of the above kind can be expected.

4. The theory of a totally entangled magnetic field, as a field in a state of maximum confusion is examined. A very close similarity between a totally entangled magnetic field and the turbulent motion in a viscous liquid is established. The question of the time of extinction of a magnetic field of a star is discussed.

Note. Sections 1, 2, 4 of the paper are based upon the results obtained by the author, reported by him at the 4th Cosmological Conference. Section 3 contains unpublished results.

Type
Part I: Magneto-Hydrodynamics
Copyright
Copyright © Cambridge University Press 1958 

References

Literaturverzeichnis

1. Cowling, T. G. M.N. 105, 166, 1945.Google Scholar
2. Lamb, H. Phil. Trans. 174, 519, 1883.Google Scholar
3. Wrubel, M. N. Astrophys. J. 116, 291, 1952.CrossRefGoogle Scholar
4. Chandrasekhar, S. Proc. Roy. Soc. A , 204, 435, 1951; 207, 301, 1951; 216, 293, 1953.Google Scholar
5. Syrovatskij, S. I., 24, 622, 1953. (Journal der Theor. und Exp. Physik, 24, 622, 1953.)Google Scholar
6. Kipper, A. (M. 1955). (Veröffentlichungen der vierten Konferenz über Fragen der Kosmogonie, Moskau, 1955.)Google Scholar
7. Batchelor, G. K. Problems of Cosmical Aerodynamics (I.A.U. Symposium, Paris), Central Air Documents Office, Dayton, Ohio, 1951.Google Scholar
8. Heisenberg, W. Problems of Cosmical Aerodynamics (I.A.U. Symposium, Paris), Central Air Documents Office, Dayton, Ohio, 1951.Google Scholar