Theoretical non-Maxwellian particle velocity distribution functions for spherically symmetric solar wind-like plasma systems and consequences

Details Theoretical non-Maxwellian particle velocity distribution functions for spherically symmetric solar wind-like plasma systems and consequences Theoretical non-Maxwellian particle velocity distribution functions for spherically symmetric solar wind-like plasma systems and consequences

Oct 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...273..363c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 273, Oct. 1, 1983, p. 363-373. Research supported by the U.S.-Israel Binati

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9

Distribution Functions, Particle Motion, Solar Wind Velocity, Variational Principles, Velocity Distribution, Anisotropy, Heat Flux, Kinetic Energy

Scientific paper

We consider spherically symmetric solar wind-like situations in which each plasma component, a (electrons, protons, alpha particles, etc.), is adequately described by the first seven moments of the velocity distribution function, fa. These moments are the particle density, radial streaming velocity, random radial kinetic energy, random transverse kinetic energy, radial transport of random radial kinetic energy, radial transport of random transverse kinetic energy, and the moment na 1 f (vr - vr )4L d3v reflecting non-Maxwellian features of the core, intermediate range, and tail particles. For such situations we use a variational principle in order to derive the most probable velocity distribution function for each component a, fa. Specifically, the derivation is based on the minimization of Boltzmann's H-function, subject to the sets of seven constraints (for each component, a) represented by the sets of seven macroscopic parameters (moments) mentioned above. For the purpose of deriving higher order fluid equations (where closure conditions and explicit expressions of particle-particle interaction terms of the Boltzmann equation are required), the result is cast into an adequate form representing an expansion (to order four) in Legendre polynomials with prescribed functional coefficients. For kinetic studies (such as electromagnetic stability analysis of the Vlasov equation or other aspects), the resulting fa is presented in a form in which the deviations from the Maxwellian are emphasized. Finally, a graphical illustration of the analytical results is presented. Subject headings: hydromagnetics - plasmas Sun: solar wind

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