Statistical properties of shock-accelerated ions in the outer heliosphere

Details Statistical properties of shock-accelerated ions in the outer heliosphere Statistical properties of shock-accelerated ions in the outer heliosphere

Oct 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...380l..93l&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 380, Oct. 20, 1991, p. L93-L96. Research supported by NASA.

Astronomy and Astrophysics

Astrophysics

7

Cosmic Rays, Heliosphere, Ion Beams, Particle Acceleration, Statistical Analysis, Interplanetary Magnetic Fields, Power Spectra, Shock Wave Propagation, Solar Wind, Voyager 2 Spacecraft

Scientific paper

Reported here are statistical studied of interplanetary protons (about 0.5-1.5 MeV) as measured by the Voyager 2 spacecraft in the outer heliosphere between about 1 and 22 AU. The acceleration processes which produce the fluctuations in intensity of the protons throughout the interval studied are caused by solar flare-generated shock waves and corotating shock structures in the solar wind. It is found that the proton count rates can be represented by a lognormal distribution, independent of the phase of the solar cycle in which the measurements were made. Power spectra of the logarithm of the counts show that for frequencies in the range of about 0.02-0.5 cycles per day, the spectra can be characterized as about f exp -2. At lower frequencies, the spectra turn over and flatten. Over the entire frequency range studied, about 0.002-0.5 cycles per day, the spectra are therefore nonfractal. The rollover in the spectra at about 100 days probably represents the reorganization time for solar wind streams within the coronal source at the sun.

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