Shock and statistical acceleration of energetic particles in the interplanetary medium

Details Shock and statistical acceleration of energetic particles in the interplanetary medium Shock and statistical acceleration of energetic particles in the interplanetary medium

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....4..162v&link_type=abstract

In NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 4 p 162-165 (SEE N85-34729 23-92)

Other

Energetic Particles, Interplanetary Medium, Particle Acceleration, Shock Waves, Solar Wind, Energy Distribution, Helios Satellites, Heliosphere, Power Spectra, Shock Fronts, Turbulence

Scientific paper

Definite evidence for particle acceleration in the solar wind came around a decade ago. Two likely sources are known to exist: particles may be accelerated by the turbulence resulting from the superposition of Alfven and Magnetosonic waves (Statistical Acceleration) or they may be accelerated directly at shock fronts formed by the interaction of fast and slow solar wind (CIR's) or by traveling shocks due to sporadic coronal mass ejections. Naurally both mechanisms may be operative. In this work the acceleration problem was tackled numerically using Helios 1 and 2 data to create a realistic representation of the Heliospheric plasma. Two 24 hour samples were used: one where there are only wave like fluctuations of the field (Day 90 Helios 1) and another with a shock present in it (Day 92 of Helios 2) both in 1976 during the STIP 2 interval. Transport coefficients in energy space have been calculated for particles injected in each sample and the effect of the shock studied in detail.

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