Polarization parameters of large-scale turbulence of the solar wind and fluctuations of the cosmic ray intensity.

Details Polarization parameters of large-scale turbulence of the solar wind and fluctuations of the cosmic ray intensity. Polarization parameters of large-scale turbulence of the solar wind and fluctuations of the cosmic ray intensity.

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991ge%26ae..31...19t&link_type=abstract

Geomagn. Aeron., Vol. 31, No. 1, p. 19 - 23

Computer Science

Interplanetary Magnetic Field: Fluctuations, Interplanetary Magnetic Field: Polarization, Cosmic Rays: Fluctuations, Cosmic Rays: Solar Modulation

Scientific paper

The method of covariant matrices is used to investigate the polarization properties of fluctuations of the interplanetary magnetic field. For three arbitrarily chosen time intervals the effective polarization parameters: the degree of polarization, the polarization angle, and the ellipticity and coherence are determined in the 10-4≤ f < 2·10-3sec-1 frequency band. It was assumed that the observed fluctuations of the IMF are representable in the form of a superposition of quasi-monochromatic waves. Analysis shows that magnetosonic waves predominate in to intervals in the polarization component of the IMF and Alfven waves in the third. It follows from a comparision of the power spectra of the fluctuations of the cosmic-ray intensity and the polarization parameters that statistically significant bursts appear in the power spectrum of fluctuations of cosmic rays with energy E > 1 GeV in the frequency band of increasing degree of polarization of magnetosonic waves.

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