Quasi-steady solar wind dynamics

Details Quasi-steady solar wind dynamics Quasi-steady solar wind dynamics

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983nascp.2280.675p&link_type=abstract

In JPL Solar Wind Five p 675-691 (SEE N84-13067 03-92)

Astronomy and Astrophysics

Astronomy

3

Dynamic Characteristics, Leading Edges, Pressure Gradients, Solar Orbits, Solar Wind, Time Dependence, Astronomical Models, Coherent Radar, Dynamic Models, Magnetic Properties, Stellar Winds, Thermodynamic Properties, Two Dimensional Models

Scientific paper

Progress in understanding the large scale dynamics of quasisteady, corotating solar wind structure was reviewed. The nature of the solar wind at large heliocentric distances preliminary calculations from a 2-D MHD model are used to demonstrate theoretical expectations of corotating structure out to 30 AU. It is found that the forward and reverse shocks from adjacent CIR's begin to interact at about 10 AU, producing new shock pairs flanking secondary CIR's. These sawtooth secondary CIR's interact again at about 20 AU and survive as visible entities to 30 AU. The model predicts the velocity jumps at the leading edge of the secondary CIR's at 30 AU should be very small but there should still be sizable variations in the thermodynamic and magnetic parameters. The driving dynamic mechanism in the distant solar wind is the relaxation of pressure gradients. The second topic is the influence of weak, nonimpulsive time dependence in quasisteady dynamics. It is suggested that modest large scale variations in the coronal flow speed on periods of several hours to a day may be responsible for many of the remaining discrepancies between theory and observation. Effects offer a ready explanation for the apparent rounding of stream fronts between 0.3 and 1.0 AU discovered by Helios.

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