Abstract
The three-fluid model equations for the solar wind are solved simultaneously in a self-consistent manner. The model consists of the individual continuity, momentum, and energy equations for electrons, protons, and ..cap alpha..-particles without considering the ..cap alpha..-particle as a minor species. The importance and the meaning of the ''critical points'' are discussed along with the proper manner of choosing them. A possible explanation for the observed streaming velocities of the ..cap alpha..-particles being larger than the proton streaming velocities is given. A weak correlation was found between the ratios of the ..cap alpha..-to-proton velocities and their temperatures near 1 AU. A definite anticorrelation between the relative ..cap alpha..-particle abundance and the particle flux was found to be in agreement with observation and in contradiction to previous theoretical models.
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