The solar wind termination shock in the presence of cosmic rays and interstellar neutrals

Details The solar wind termination shock in the presence of cosmic rays and interstellar neutrals The solar wind termination shock in the presence of cosmic rays and interstellar neutrals

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997adspr..19..961z&link_type=abstract

Advances in Space Research, Volume 19, Issue 6, p. 961-964.

Physics

1

Scientific paper

The cosmic ray mediated solar wind model is presented, in which the interplanetary magnetic field and the interaction with interstellar matter is taken into account. For a given position of the termination shock a set of solar wind hydrodynamic equations and pressure equations for galactic and anomalous cosmic rays is solved in the range [1,200] AU. The obtained velocity and pressure profiles are studied in dependence on: (i) solar wind parameters at 1 AU, (ii) pickup ions production rate, (iii) diffusion coefficients of cosmic rays. The models are constrained by the solar wind pressure at the heliopause P_LISM = 1 eV/cm^3, and the galactic cosmic rays pressure in the interstellar medium P^G = 0.33 eV/cm^3. These constraints limit the shock position in the ecliptic to 80-90 AU and the production efficiency of anomalous cosmic rays at the shock to about 10%.

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