Previous abstract Next abstract

Session 14 - Solar-Terrestrial, Solar Wind.
Oral session, Monday, June 30
Ballroom A, Chair: David Webb

[14.06] A Re-examination of the Parker Solar Wind Model

T. G. Moran (NASA/GSFC)

The solar wind cannot be explained by the original or modified versions of the Parker model. In the absence of a time-varying driving force the corona would be found in a static,convective state, or a subsonic expansion state, rather than the state of constant, supersonic expansion predicted by the Parker model. According to the Parker model, the corona expands with a velocity following a particular solution of the undriven, steady-state fluid equations from a specific subsonic velocity at the sun, reaching the sound speed at the 'critical point' and becoming supersonic beyond the critical point. Parker argued that the corona must expand according to this solution since there are no other physical solutions to the undriven, steady-state fluid equations. However, we reinvestigate static and subsonic solutions and find solutions of these types which are physical and therefore must be considered as possible equilibrium states. By applying the second law of thermodynamics we determine the equilibrium state for a corona with no driving force, and with a constant driving force, and demonstrate that the solar wind must be driven by a time-dependent force, and therefore the solar wind itself must be time-varying.


The author(s) of this abstract have provided an email address for comments about the abstract: moran@orpheus.nascom.nasa.gov

Program listing for Monday