Solar wind proton velocity distributions - Comparison of the bi-Maxwellian based 16-moment expansion with observations

Details Solar wind proton velocity distributions - Comparison of the bi-Maxwellian based 16-moment expansion with observations Solar wind proton velocity distributions - Comparison of the bi-Maxwellian based 16-moment expansion with observations

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990p%26ss...38.1091d&link_type=abstract

Planetary and Space Science (ISSN 0032-0633), vol. 38, Sept. 1990, p. 1091-1103.

Physics

8

Interplanetary Magnetic Fields, Solar Protons, Solar Wind Velocity, Velocity Distribution, Distribution Functions, Magnetic Field Configurations, Normal Density Functions, Particle Energy

Scientific paper

The purpose of this paper is to study the possible types of velocity distributions that can be obtained from the bi-Maxwellian based 16-moment expansion of the distribution function, assuming macroscopic parameter values characteristic of the range of solar wind conditions. While previous studies also took heat flow into account, the theoretical expansions for f and the definitions of the physical moments adopted in these studies were different from those used in this paper. The choice of the 16-moment expansion and corresponding moment definitions was motivated by the fact that this is the correct generalization of the widely-used Maxwellian-based 13-moment expansion to the case where the zeroth-order distribution is a bi-Maxwellian. It is found that most of the features characteristic of solar wind proton distributions can be reproduced with the 16-moment distribution, including the appearance of secondary peaks. It is also shown how each of the physically significant velocity moments affects the shape of the distribution function.

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