Perturbation of the solar wind in a model terrestrial foreshock

Details Perturbation of the solar wind in a model terrestrial foreshock Perturbation of the solar wind in a model terrestrial foreshock

Aug 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986jgr....91.8798s&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 91, Aug. 1, 1986, p. 8798-8804.

Physics

4

Earth Magnetosphere, Magnetohydrodynamic Flow, Plasma Oscillations, Shock Fronts, Solar Terrestrial Interactions, Solar Wind, Linear Equations, Magnetic Flux, Pressure Distribution, Two Dimensional Flow

Scientific paper

The perturbation of the solar wind in the earth's foreshock is studied, with the foreshock modeled as a planar magnetic tube with a 15-earth-radii half-width along the bow shock. The upstream energetic particle pressure perturbs the incoming solar wind, and the perturbations are derived using the steady state ideal MHD equations. The vector solar wind velocity perturbation is seen to rotate from the sunward to the transverse direction with increasing distance from the axis of the flux tube, and the peak solar wind deflection is located three earth radii within the flux tube boundary. A central upstream pressure of 200 eV/cu cm is found to produce a maximum deceleration of 6 km/s and a maximum deflection of 3.6 deg. Perturbations of the solar wind density and the magnetic field, accompanying the noted deflection and deceleration, are largest near the flux tube boundary where both form spikes having a width of about 2 earth radii. The solutions of the linearized flow problem are reduced to quadrature.

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