Magnetohydrodynamic interaction of highspeed streams
Abstract
Numerical solutions of a magnetohydrodynamic model are carried out to describe the nonlinear interaction of corotating highspeed streams near the solar equatorial plane. Two problems are studied. The first problem is to simulate the evolution of an idealized highspeed stream. Numerical solutions are obtained to represent the variations of flow velocity, magnetic field, plasma density, temperature, and conduction heat flux in the interaction region. They demonstrate that the dynamical interaction and heat conduction process are responsible for the thermal structure of a highspeed stream. The second problem deals with the formation of corotating shock waves near the leading edge of a broad stream resulting from the merging of characteristic curves. Corotating shocks do not necessarily occur in pairs; a reverse shock can be formed without a forward shock nearby.
 Publication:

Journal of Geophysical Research
 Pub Date:
 May 1981
 DOI:
 10.1029/JA086iA05p03263
 Bibcode:
 1981JGR....86.3263W
 Keywords:

 Astronomical Models;
 Interplanetary Medium;
 Magnetohydrodynamic Flow;
 Plasma Interactions;
 Solar Wind;
 Cosmic Plasma;
 Ecliptic;
 Flow Velocity;
 High Speed;
 Magnetic Field Configurations;
 Magnetohydrodynamic Stability;
 Numerical Analysis;
 Plasma Density;
 Plasma Temperature;
 Shock Wave Interaction;
 Thermal Conductivity;
 Solar Physics