A time-dependent two-fluid model with thermal conduction for the solar wind

Details A time-dependent two-fluid model with thermal conduction for the solar wind A time-dependent two-fluid model with thermal conduction for the solar wind

Aug 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...231..960m&link_type=abstract

Astrophysical Journal, Part 1, vol. 231, Aug. 1, 1979, p. 960-976.

Astronomy and Astrophysics

Astrophysics

9

Solar Wind, Thermal Conductivity, Time Dependence, Two Fluid Models, Electron Energy, Graphs (Charts), Numerical Integration, Perturbation Theory, Proton Energy, Shock Wave Propagation, Steady State

Scientific paper

A time-dependent spherically symmetric two-fluid model for the solar wind is presented. The model simultaneously solves continuity, momentum, and energy equations and incorporates thermal conduction for both electron and proton components with allowance for noncollisional modifications. One-fluid and two-fluid time-dependent solutions with and without consideration of thermal conduction effects are studied, and the influence of various perturbations superposed on the steady-state solar-wind plasma at the inner boundary (10 solar radii) is also investigated. It is found that as in the steady-state case, the unique temperature of the one-fluid time-dependent case represents to a good approximation the electron temperature of the two fluid time dependent case. Secondly, in the two-fluid time-dependent case, just as in the one-fluid case, a shock is formed in the interplanetary medium when higher speed solar wind streams overtake the lower speed steady solar wind. Finally, the time-dependent solutions of the two-fluid model provide proton to electron temperature ratios. It is concluded that these results are relevant for both long-lived corotating high speed solar wind streams and short-lived phenomena.

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