Solar wind electrons: Parametric constraints

Details Solar wind electrons: Parametric constraints Solar wind electrons: Parametric constraints

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999jgr...10419843g&link_type=abstract

Journal of Geophysical Research, Volume 104, Issue A9, p. 19843-19850

Physics

9

Interplanetary Physics: Solar Wind Plasma

Scientific paper

Solar wind electrons are often observed to consist of two distinguishable components, a thermal, more dense core and a suprathermal, less dense halo. In this core/halo model linear Vlasov theory for the whistler heat flux instability predicts dimensionless heat flux thresholds which decrease as the electron core beta, β~∥c, increases. It has been proposed that this theoretical threshold corresponds to an observable upper bound on the electron heat flux. Linear theory also predicts that there is a critical value of β~∥c below which the whistler heat flux instability does not have appreciable growth in the solar wind; there is another suggestion that this corresponds to an observable lower bound on β~∥c. These two proposals are examined by comparison of linear theory and data from the initial in-ecliptic phase of the Ulysses mission. The instability threshold does provide a statistical constraint on observed solar wind heat fluxes, and the critical β~∥c of theory is not inconsistent with a statistical lower bound on the observations of that parameter.

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