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Cosmic Rays and the Parker Instability

Published online by Cambridge University Press:  04 August 2017

A.H. Nelson
A.H. Nelson*
Affiliation:
Dept. of Applied Mathematics & Astronomy, University College Cardiff, U.K.

Extract

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Parker (1966, 1969, 1979) has shown that the magnetic buoyancy of a uniform horizontal magnetic field will destabilize the Galactic gas layer. Perturbations of the form shown in Fig. 1 will grow in time with the magnetic loops ballooning up into the Galactic halo, and the interstellar gas draining down the field lines to collect in the mid-plane. Parker also showed that if the dynamical effect of the cosmic ray component of the interstellar medium is included, using an isotropic cosmic ray pressure, then the instability is enhanced.

Type
Session V
Information
Symposium - International Astronomical Union , Volume 107: Unstable Current Systems and Plasma Instabilities , 1985 , pp. 361 - 363
Copyright
Copyright © Reidel 1985 

References

Chew, G.F., Goldberger, M.O., and Low, F.E.: 1956, Proc. Roy. Soc. A236, 112.Google Scholar
Mouschovias, T. Ch., Shu, F.H., and Woodward, P.R.: 1974, Astron. Astrophys. 33, 73.Google Scholar
Parker, E.N.: 1966, Ap. J. 145, 811.Google Scholar
Parker, E.N.: 1967, Ap. J. 149, 535.Google Scholar
Parker, E.N.: 1969, Space Sci. Rev. 9, 651.Google Scholar
Parker, E.N.: 1979, Cosmical Magnetic Fields, Clarendon Press, Oxford.Google Scholar
Rossi, B. and Olbert, S.: 1970, Introduction to the Physics of Space, pp.354–358, McGraw–Hill.Google Scholar
Shu, F.H.: 1983, I.A.U. Symp 106.Google Scholar