An analytical solution for the heliopause boundary and its comparison with numerical solutions

Details An analytical solution for the heliopause boundary and its comparison with numerical solutions An analytical solution for the heliopause boundary and its comparison with numerical solutions

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...255..383r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 255, no. 1-2, p. 383-387.

Astronomy and Astrophysics

Astrophysics

8

Heliosphere, Hypersonic Flow, Magnetohydrodynamics, Plasma Interactions, Solar Wind, Space Plasmas, Astronomical Models, Boundary Layers, Bow Waves, Interstellar Magnetic Fields, Shock Waves

Scientific paper

A comparison of different heliopause configurations obtained by using the Newtonian approximation (NA) or the Parker's solution for a plasma-plasma type interface with the complete hydrodynamic calculations (Baranov et al., 1979) shows that there exists a domain in which the Parker solution is very close to that obtained by NA and in which both are close to the Baranov et al. (1979) solution for the inner bow shock. This leads to the idea of using the analytic form of Parker's solution (for subsonic flows) as the approximate solution for just the opposite case, namely, the interaction between two hypersonic streams. By this means, treating the compressible layers between the two bow shocks as a thin layer and assuming the plasma velocity as a constant throughout the cross dimension of the shock layer, a third-order ordinary differential equation describing the heliopause is obtained. This equation is then solved numerically. An analytical solution of this equation on the basis of a Parker type solution is also found, which is then used to develop a simple procedure for describing the heliospheric interface.

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