Slow shocks and their transition to fast shocks in the inner solar wind

Details Slow shocks and their transition to fast shocks in the inner solar wind Slow shocks and their transition to fast shocks in the inner solar wind

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987jgr....92.4349w&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 92, May 1, 1987, p. 4349-4356.

Physics

39

Interplanetary Space, Magnetohydrodynamic Waves, Plasma Density, Shock Wave Propagation, Solar Wind, Heliosphere, Solar Corona

Scientific paper

The jump conditions of MHD shocks may be directly calculated as functions of the shock Alfven number based on the normal component of the relative shock speed, the shock angle, and the plasma beta value. A traveling, forward shock can be a slow shock in coronal space, where the Alfven speed is of the order of 1000 km/s. The surface of a forward slow shock has a bow-shaped geometry with its nose facing toward the sun. The decrease in the Alfven speed at increasing heliocentric distance causes the shock Alfven number of a forward slow shock to become greater than 1, and the shock eventually evolves from a slow shock into a fast shock. As the system moves outward from the sun, the area enclosed by the transition line expands, the fast shock grows stronger, and the slow shock becomes weaker. Eventually, the slow shock diminishes, and the entire shock system evolves into a forward fast shock.

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