A forward-reverse shock pair in the solar wind driven by over-expanison of a coronal mass ejection: ULYSSES observations

Details A forward-reverse shock pair in the solar wind driven by over-expanison of a coronal mass ejection: ULYSSES observations A forward-reverse shock pair in the solar wind driven by over-expanison of a coronal mass ejection: ULYSSES observations

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994georl..21..237g&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 21, no. 3, p. 237-240

Physics

53

Shock Waves, Solar Corona, Solar Magnetic Field, Solar Physics, Solar Wind, Stellar Mass Ejection, Sun, Electrons, Mathematical Models, Solar Activity, Ulysses Mission

Scientific paper

A previously unidentified type of solar wind forward-reverse shock pair has been observed by Ulysses at 4.64 AU and S32.5 deg. In contrast to most solar wind forward-reverse shock pairs, which are driven by the speed difference between fast solar wind plasma and slower plasma ahead, this particular shock pair was driven purely by the over-expansion of a coronal mass ejection (CME) in transit from the Sun. A simple numerical simulation indicates that the over-expansion was a result of a high initial internal plasma and magnetic field pressure within the CME. The CME observed at 4.64 AU had the internal field structure of a magnetic flux rope. This event was associated with a solar disturbance in which new magnetic loops formed in the corona almost directly beneath Ulysses approximately 11 days earlier. This association suggests that the flux rope was created as a result of reconnection between the 'legs' of neighboring magnetic loops within the rising CME.

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