Solar-wind properties at the Earth as predicted by the two-fluid model |
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| Authors: | B R Durney |
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| Institution: | 1. Advanced Study Program, National Center for Atmospheric Research, Boulder, Colo., U.S.A.
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| Abstract: | The two-fluid equations for the solar wind are written down in a simplified form, similar to that suggested by Roberts (1971) for the one-fluid model. The equations are shown to depend only on one parameter, $$K = GM\kappa _e m_p (\varepsilon _\infty T_0 )^{{3 \mathord{\left/ {\vphantom {3 2}} \right. \kern-\nulldelimiterspace} 2}} /4k^2 Fe,$$ , where G is the gravitational constant, M the mass of the star, κ e the thermal electron conductivity, m p the proton mass, k the Boltzman constant, k? ∞T0 the residual energy per particle at infinity and F e the electron-particle flux. For a variety of values of the density and temperature at the base of the corona we compute the solutions of the two-fluid solar wind model and compare the predicted and observed solar wind parameters at the Earth. |
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