Flow downstream of the heliospheric terminal shock - Magnetic field kinematics

Details Flow downstream of the heliospheric terminal shock - Magnetic field kinematics Flow downstream of the heliospheric terminal shock - Magnetic field kinematics

Oct 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...250..556n&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 250, no. 2, Oct. 1991, p. 556-564.

Astronomy and Astrophysics

Astrophysics

25

Heliosphere, Interplanetary Magnetic Fields, Interstellar Matter, Lines Of Force, Shock Wave Propagation, Solar Wind, Magnetohydrodynamics, Solar Neighborhood

Scientific paper

A kinematic model of the interplanetary magnetic field in the heliosheath beyond the solar wind terminal shock is presented in order to evaluate the possible importance of MHD effects in that region of space. The need for this evaluation arises because the interplanetary magnetic field is compressed across the terminal shock and further amplified by the decreasing flow speed beyond the shock. Streamlines which approach the stagnation point before turning in the downstream direction lead to the strongest effects due to the extreme slowing of the solar wind and consequent compression of the embedded magnetic field. The magnetic volume force therefore cannot be neglected on streamlines that approach the heliopause in the upstream direction, where the volume containing them is a large fraction of the overall of the heliosheath in the upstream direction. The increase in the magnetic pressure may act to bring the upstream terminal shock significantly closer to the sun, potentially reconciling a conflict between models and observations.

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