Three-dimensional MHD simulation of the April 14, 1994, interplanetary coronal mass ejection and its propagation to Earth and Ulysses

Details Three-dimensional MHD simulation of the April 14, 1994, interplanetary coronal mass ejection and its propagation to Earth and Ulysses Three-dimensional MHD simulation of the April 14, 1994, interplanetary coronal mass ejection and its propagation to Earth and Ulysses

Jul 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997jgr...10214065d&link_type=abstract

Journal of Geophysical Research, Volume 102, Issue A7, p. 14065-14074

Astronomy and Astrophysics

Astrophysics

12

Interplanetary Physics: Interplanetary Shocks, Interplanetary Physics: Solar Wind Plasma, Magnetospheric Physics: Solar Wind/Magnetosphere Interactions, Solar Physics, Astrophysics, And Astronomy: Coronal Mass Ejections

Scientific paper

A three-dimensional (3-D), time-dependent, magnetohydrodynamic (MHD) model is used to simulate the interplanetary propagation of a disturbance that started in the low corona via the destabilization of a southern hemisphere helmet-streamer on April 14, 1994. A severe geomagnetic storm occurred at Earth, and a forward-reverse shock structure was detected at Ulysses (3.2 AU) at E30°S60°. The model is initiated at 18Rs (where Rs is the solar radius, 6.95×105km) within the supersonic and super-Alfvenic region of the solar wind; hence no consideration is given to the disturbance's evolution from ~1Rs to 18Rs. We refer to the interplanetary disturbance as an interplanetary/coronal mass ejection (ICME) to indicate that it may be relevant to what has been referred to in the literature as a CME but is not related to the flux rope or magnetic cloud that has also received much attention. We find that the 3-D MHD model, with a simple pressure pulse (suggested by Yohkoh soft Xray observations), provides a satisfactory comparison with the SSC timing at Earth and the Ulysses observations.

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