Numerical simulation of the 12 May 1997 interplanetary CME event

Details Numerical simulation of the 12 May 1997 interplanetary CME event Numerical simulation of the 12 May 1997 interplanetary CME event

Feb 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004jgra..10902116o&link_type=abstract

Journal of Geophysical Research, Volume 109, Issue A2, CiteID A02116

Astronomy and Astrophysics

Astrophysics

51

Solar Physics, Astrophysics, And Astronomy: Coronal Mass Ejections, Interplanetary Physics: Ejecta, Driver Gases, And Magnetic Clouds, Interplanetary Physics: Solar Wind Plasma, Mathematical Geophysics: Numerical Solutions

Scientific paper

Numerical three-dimensional magnetohydrodynamic models are capable of predicting large-scale solar wind structures at Earth, provided that appropriate time-dependent boundary conditions are specified near the Sun. Since knowledge of such conditions is at present insufficient to directly drive the models, various approximations are used. In this paper, we introduce the main features and approximations of a numerical model where (1) the ambient solar wind is derived from coronal models utilizing photospheric magnetic field observations and (2) transient disturbances are derived from geometrical and kinematic fitting of coronagraph observations of coronal mass ejections (CMEs). We have chosen the well-defined halo-CME event of 12 May 1997 as our initial event because it is characterized by a relatively quiet solar and interplanetary background into which the ejecta was launched. The numerical simulation has enabled us to predict the arrival of the shock and ejecta and provided us with a global picture of transient disturbance interacting with a moderately fast solar wind stream.

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