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• W2146182376 startingPage "3137" @default.
• W2146182376 abstract "A three‐fluid model for the solar wind, with continuity, momentum, and energy equations for the three species protons, alpha particles, and electrons, including electron heat conduction and a parameterized coronal heat source, is used to study the behavior of the resulting proton and alpha fluxes as a function of coronal energy input and the proton‐to‐alpha density ratio at the coronal base. While in model solutions without alpha particles the proton flux is a strongly increasing function of coronal temperature, quite opposite to the observed near constancy of the proton flux in the solar wind, solutions with alpha particle abundances of the order of a few percent at the coronal base have a reduced proton flux and much less variation of the proton flux. The mechanism by which the proton flux is reduced is a pileup of the alpha particle abundance in the region of the coronal temperature maximum and the increased frictional drag on the protons resulting therefrom. We find a range of model solutions in which the resulting proton flux is almost independent of coronal energy input or coronal temperature, and we conclude that proton‐alpha friction and dynamic accumulation of alphas in the corona can provide an explanation for the near constancy of the proton flux which is observed in the solar wind." @default.
• W2146182376 created "2016-06-24" @default.
• W2146182376 creator A5075922717 @default.
• W2146182376 date "1992-03-01" @default.
• W2146182376 modified "2023-09-27" @default.
• W2146182376 title "Proton and alpha particle fluxes in the solar wind: Results of a three-fluid model" @default.
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• W2146182376 doi "https://doi.org/10.1029/91ja02833" @default.
• W2146182376 hasPublicationYear "1992" @default.
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