Steady-state magnetic field in the magnetosheath

Details Steady-state magnetic field in the magnetosheath Steady-state magnetic field in the magnetosheath

May 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982p%26ss...30..473k&link_type=abstract

Planetary and Space Science, vol. 30, May 1982, p. 473-481.

Computer Science

9

Bow Waves, Geomagnetism, Magnetopause, Magnetoplasmadynamics, Magnetosheath, Planetary Magnetic Fields, Shock Waves, Solar Wind, Gas Dynamics, Magnetohydrodynamic Flow, Plasma-Electromagnetic Interaction, Solar Terrestrial Interactions, Spacecraft Trajectories, Steady State, Three Dimensional Flow, Transition Layers

Scientific paper

The magnetic field in the transition region between the bow shock and the effective obstacle, in steady-state, three-dimensional solar wind flow around a planet, is found by a numerical method in which, on the assumption that the Alfven-Mach number is very large, there is a decoupling into gasdynamic and electromagnetic problems. The gasdynamic problem is solved in the axisymmetric formulation, and the equations for the magnetic field are solved numerically. After comparison with previous solutions, the results are discussed with a view to satellite data interpretation.

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