CME Evolution in the Corona and Solar Wind

Details CME Evolution in the Corona and Solar Wind CME Evolution in the Corona and Solar Wind

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh61a0433l&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH61A-0433

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Computation

2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields, 7513 Coronal Mass Ejections, 7524 Magnetic Fields

Scientific paper

Coronal mass ejections (CMEs), immense eruptions of plasma and magnetic fields with velocities as high as 2000 km/s, are a major transient input of mass and energy into the solar wind. We are using time-dependent 2D and 3D MHD computations to study the evolution of CMEs. A simulated CME is initiated by flux cancellation at the photosphere. The calculation follows the eruption and the subsequent propagation of a magnetic flux rope to 1 AU. We discuss the evolutionary properties of the CME, both near the Sun and beyond the Alfven and sonic points. We also examine the properties likely to be inferred about the flux rope from simulated time series data obtained when the flux rope passes over hypothetical spacecraft at different positions. Work supported by NASA and NSF.

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