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Stability of the solar wind against the whistler mode

Published online by Cambridge University Press:  13 March 2009

P. Revathy
P. Revathy
Affiliation:
Indian Institute of Geornagnetism, Colaba, Bombay 400 005, India
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Abstract

The stability of the solar wind against the whistler mode is analyzed. It is shown that the solar wind can become unstable owing to this mode after a distance of 100 R from the sun. The minimum value of the relative velocity (Ur) between ∝-particles and protons for the excitation of this instability is the proton thermal velocity αi. The maximum growth rate at 200 R occurs for the values of the parameters kρi = 0·3,(T┤/T∥)i = 0·3 and Ur/αi = 0·5.

Type
Research Article
Information
Journal of Plasma Physics , Volume 20 , Issue 2 , October 1978 , pp. 225 - 230
Copyright
Copyright © Cambridge University Press 1978

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References

REFERENCES

Asbridge, J. R., Bame, S. J. & Feldman, W. C. 1973 EOS Trans. AGU. 54, 440.Google Scholar
Bame, S. J., Asbrider, J. R., Feldman, W. C., Gary, S. P. & Montgomery, M. D. 1975 Geophys. Res. Lett. 2, 373.CrossRefGoogle Scholar
Bollea, D. V., Formisano, F. C., Hedgecock, G., Moreno, G. & Pelmiotte, F. 1972 Solar Wind, pp. 308, 588. NASA Special Publications.Google Scholar
Buti, B. 1973 a Astrophys. J. 181, 1055.CrossRefGoogle Scholar
Buti, B. 1973 b J. Geophys. Res. 78, 8023.CrossRefGoogle Scholar
Feldman, W. C., Asbrideg, J. R., Bame, S. J. & Montgomery, M. D. 1973 J. Geophys. Res. 78, 2017.CrossRefGoogle Scholar
Feldman, W. C., Asbrideg, J. R., Bame, S. J., Gary, S. P. & Montgomery, M. D. 1976 J. Geophys. Res. 81, 2377.CrossRefGoogle Scholar
Formisano, V. & Moreno, G. 1971 Riv. Nuovo Cimento, 1, 365.CrossRefGoogle Scholar
Fredricks, R. W. & Scarf, F. L. 1965 J. Geophys. Res. 70, 4765.CrossRefGoogle Scholar
Fried, B. D. & Conte, S. D. 1961 The Plasma Dispersion Function. Academic.Google Scholar
Geiss, J., Hirt, P. & Leutwyler, H. 1970 Solar Phys. 12, 458.CrossRefGoogle Scholar
Hirshberg, J., Aaberidge, J. R. & Robbins, D. E. 1974 J. Geophys. Res. 79, 934.CrossRefGoogle Scholar
Hundhausen, A. J. 1970 Rev. Geophys. Space Phys. 8, 729.CrossRefGoogle Scholar
Lakhina, G. S. & Buti, B. 1976 J. Geophys. Res. 81, 2135.CrossRefGoogle Scholar
Montgomery, M. D. 1972 Solar Wind, p. 208. NASA Special Publications.Google Scholar
Montgomery, M. D., Gary, S. P., Feldman, W. C. & Forslund, D. W. 1976 J. Geophys. Res. 81, 2743.Google Scholar
Revathy, P. 1977 Symposium on Magnetospheric Physics, Indian Institute of Geomagnetism, Bombay.Google Scholar
Robbins, D. E., Hundhausen, A. J. & Bame, S. J. 1970 J. Geophys. Res. 75, 1178.CrossRefGoogle Scholar
Scharer, J. E. & Trivelpiece, A. W. 1967 Phys. Fluids, 10, 591.CrossRefGoogle Scholar