On the origin of long time-scale pulsar scintillations. I - Cosmic ray streaming or the mirror instability. II - Growth of the mirror instability, and non-linear amplitude limitation. III - The density fluctuations in our Galaxy

Details On the origin of long time-scale pulsar scintillations. I - Cosmic ray streaming or the mirror instability. II - Growth of the mirror instability, and non-linear amplitude limitation. III - The density fluctuations in our Galaxy On the origin of long time-scale pulsar scintillations. I - Cosmic ray streaming or the mirror instability. II - Growth of the mirror instability, and non-linear amplitude limitation. III - The density fluctuations in our Galaxy

Feb 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980mnras.190..353h&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 190, Feb. 1980, p. 353-369, 371-383, 385-393. Research supported by the

Astronomy and Astrophysics

Astronomy

18

Astronomical Models, Magnetohydrodynamic Stability, Milky Way Galaxy, Pulsars, Scintillation, Cosmic Rays, Gas Density, Interstellar Gas, Larmor Precession, Nonlinearity, Spectrum Analysis

Scientific paper

The present analysis refutes the suggestion that cosmic rays streaming along the magnetic fields of the Galaxy produce the small-scale density fluctuations in the interstellar medium, responsible for long time-scale pulsar scintillations. A discussion of the turbulence in the hot component of the interstellar medium reveals it as a source of pressure anisotropies which render the plasma either firehose or mirror unstable. Application of a magnetohydrodynamic analysis to these instabilities leads to the conclusion that mirror instabilities appear to be responsible for the small-scale density fluctuations. It is shown that mirror instabilities can give a satisfactory account of both the scale length and amplitude of the density fluctuations. The form of the spectrum of the density fluctuations is examined.

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