Interaction of interplanetary shocks with the heliospheric termination shock: Two-dimensional magnetohydrodynamic model

Details Interaction of interplanetary shocks with the heliospheric termination shock: Two-dimensional magnetohydrodynamic model Interaction of interplanetary shocks with the heliospheric termination shock: Two-dimensional magnetohydrodynamic model

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996jgr...10127465b&link_type=abstract

Journal of Geophysical Research, Volume 101, Issue A12, p. 27465-27482

Physics

8

Interplanetary Physics: Discontinuities, Interplanetary Physics: Heliopause And Solar Wind Termination, Interplanetary Physics: Interplanetary Shocks, Interplanetary Physics: Solar Wind Plasma

Scientific paper

The two-dimensional problem of the oblique interaction between an interplanetary shock (IPS) and the termination shock (TS) with allowance for the effect of the interplanetary magnetic field is studied within the framework of the ideal magnetohydrodynamic model and a steady model of the solar wind interaction with the local interstellar medium. The self-consistent axisymmetric model proposed by Baranov and Malama which takes into account the processes of resonant charge exchange between H atoms and protons is used. The electron number density and the solar wind velocity VSW ahead of TS depends on the parameters of this model. The postinteraction configuration consists of a new moving TS', a transmitted IPS', a set of Alfvén and slow magnetohydrodynamic waves, and a contact discontinuity which can change as functions of five dimensionless governing parameters and the specific heat ratio γ. The maximum electron number density ne is usually reached behind the new termination shock TS' for an oblique (θ≠0) impingement of IPS on TS rather than for the head-on collision (θ=0). Nevertheless, the maximum calculated values of ne are lower than those corresponding to plasma frequencies ωp≃2kHz observed by the Voyager spacecraft. It is found that all the quantities considered depends radically on the angle ψTS between the front of TS and the vector of the interplanetary magnetic field strength BSW.

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