Computer Science – Numerical Analysis
Scientific paper
Jul 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..152..457u&link_type=abstract
Solar Physics, vol. 152, no. 2, p. 457-479
Computer Science
Numerical Analysis
9
Applications Of Mathematics, Current Sheets, Explosions, Heliosphere, Magnetohydrodynamic Waves, Mathematical Models, Numerical Analysis, Shock Fronts, Shock Wave Propagation, Shock Waves, Solar Wind, Wave Front Deformation, Wave Propagation, Wentzel-Kramer-Brillouin Method, Magnetic Field Configurations, Nonlinearity, Plasma Density, Solar Flares, Waveguides
Scientific paper
The interplanetary shock wave front shape and intensity are calculated numerically by means of the Wentzel-Kramer-Brillouin (WKB)-approach, with nonlinear effects taken into account. The solar flare is modelled as an isotropic point explosion at the solar wind base. The heliospheric current sheet (HCS) is represented by a radially diverging stream with a higher plasma concentration and a lower wind speed. Fast magnetosonic shock wave propagation along the HCS is connected with the effect of regular accumulation of the wave energy in the vicinity of the HCS. In this place the wave intensity is increased, and the corresponding front fragments go ahead to form a shock-wave forerunner as a 'pimple'. The 'pimple', in turn, is located inside quite a large, but less-contrast, 'dimple' in the wave surface. This 'dimple' approximately coincides with the HCS stream contours. If the flare is outside the HCS boundaries, the picture discussed above is conserved, but asymmetry effects arise. Thus the interplanetary shock is stronger when the Earth's observer and the flare are on the same side of the HCS and is weaker in the opposite case.
Uralov Arkadiy M.
Uralova S. V.
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