The evolution of corotating stream fronts near the ecliptic plane in the inner solar system. I - Two-dimensional fronts

Details The evolution of corotating stream fronts near the ecliptic plane in the inner solar system. I - Two-dimensional fronts The evolution of corotating stream fronts near the ecliptic plane in the inner solar system. I - Two-dimensional fronts

Jul 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989jgr....94.8673p&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 94, July 1, 1989, p. 8673-8684.

Physics

29

Corotation, Rotating Plasmas, Solar Wind, Two Dimensional Models, Flow Characteristics, Magnetohydrodynamic Flow, Shock Fronts, Supersonic Flow

Scientific paper

Numerical models of corotating solar wind flows tend to predict that corotating shock pairs should occur relatively frequently within 1 AU. This paper uses an existing two-dimensional MHD numerical model for corotating flow in the supersonic super-Alfvenic solar wind to demonstrate that the predictions of previous models with respect to the steepening of stream fronts within 1 AU are due to improper specification of the flow conditions on the initial surface (inner boundary) used as the starting point in these models. An initialization scheme is presented, that incorporates flow conditions more appropriate to the stream fronts near the sun, which is shown to produce the smooth initial behavior expected on physical grounds. In this scheme, criteria for shock formation are described in terms of the interface dynamics. It is shown that the steepening process cannot be treated even approximately with conventional kinematic techniques.

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