Solar-Wind Properties at the Earth as Predicted by the Two-Fluid Model
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 = GMκemp (ɛ&inftyT0)3/2/4k2 Fe, where G is the gravitational constant, M the mass of the star, κe the thermal electron conductivity, mp the proton mass, k the Boltzman constant, kɛ∞T0 the residual energy per particle at infinity and Fe 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.
- Publication:
-
Solar Physics
- Pub Date:
- May 1973
- DOI:
- 10.1007/BF00156191
- Bibcode:
- 1973SoPh...30..223D
- Keywords:
-
- Solar Wind;
- Electron Conductivity;
- Residual Energy;
- Gravitational Constant;
- Wind Model