Overexpanding coronal mass ejections at high heliographic latitudes - Observations and simulations

Details Overexpanding coronal mass ejections at high heliographic latitudes - Observations and simulations Overexpanding coronal mass ejections at high heliographic latitudes - Observations and simulations

Feb 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998jgr...103.1941g&link_type=abstract

Journal of Geophysical Research, vol. 103, p. 1941

Physics

53

Solar Corona, Coronal Mass Ejection, Ulysses Mission, Solar Wind, Radial Distribution, Refracted Waves, Plasma Pressure

Scientific paper

Ulysses observations reveal that most coronal mass ejections (CMEs) observed in the solar wind far from the sun at high heliographic latitudes have large radial widths and are still expanding as they pass the spacecraft. CME radial widths ranging between 0.5 and 2.5 AU have been observed at heliocentric distances between 1.4 and 4.6 AU and at latitudes greater than 22 deg. A CME may expand simply because it is ejected from the sun with a leading edge speed that is greater than its trailing-edge speed. Rarefaction waves produced by relative motion between a CME and the surrounding wind also can cause a CME to expand. Finally, a CME may expand because it is ejected into the wind with an internal pressure that is greater than that of the surrounding wind. In the latter case, which we have called 'overexpansion', the expansion tends to drive compressive waves into the surrounding solar wind; these waves commonly steepen into shocks at large distances from the sun. Using Ulysses observations and a simple 1D, gasdynamic code, we have explored how initial conditions affect the radial evolution of solar wind disturbances associated with overexpanding CMEs. We find good qualitative agreement between the results of our simulations and Ulysses observations of such disturbances.

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