Termination of the solar wind in the hot, partially ionized interstellar medium

Details Termination of the solar wind in the hot, partially ionized interstellar medium Termination of the solar wind in the hot, partially ionized interstellar medium

Nov 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974phdt.........1l&link_type=abstract

Ph.D. Thesis Stanford Univ., CA.

Computer Science

1

Interstellar Matter, Ionized Gases, Solar Wind, Computer Programming, Magnetohydrodynamics, Photoionization

Scientific paper

Theoretical foundations for understanding the problem of the termination of the solar wind are reexamined in the light of most recent findings concerning the states of the solar wind and the local interstellar medium. The investigation suggests that a simple extention of Parker's (1961) analytical model provides a useful approximate description of the combined solar wind, interstellar wind plasma flowfield under conditions presently thought to occur. A linear perturbation solution exhibiting both the effects of photoionization and charge exchange is obtained for the supersonic solar wind. A numerical algorithm is described for computing moments of the non-equilibrium hydrogen distribution function and associated source terms for the MHD equations. Computed using the algorithm in conjunction with the extended Parker solution to approximate the plasma flowfield, profiles of hydrogen number density are given in the solar wind along the upstream and downstream axes of flow with respect to the direction of the interstellar wind. Predictions of solar Lyman-alpha backscatter intensities to be observed at 1 a.u. have been computed, in turn, from a set of such hydrogen number density profiles varied over assumed conditions of the interstellar wind.

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