Understanding the Evolution of Coronal Mass Ejections in the Interplanetary Space (Invited)

Details Understanding the Evolution of Coronal Mass Ejections in the Interplanetary Space (Invited) Understanding the Evolution of Coronal Mass Ejections in the Interplanetary Space (Invited)

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh43c..04z&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH43C-04

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7924] Space Weather / Forecasting

Scientific paper

The evolution of coronal mass ejections (CMEs) in the interplanetary space is now well observed by STEREO and SOHO from multiple vantage points in space. Knowledge of CME propagation is further gained by in-situ observations. Using the six-parameter graduated cylindrical shell (GCS) model, we track several major CMEs from solar surface to a large distance into the interplanetary space, and study their detailed evolution in 3-D space. We report (1) how the leading edge (LE) velocity changes with distance, which seems to follow an exponential function with time, (2) how the expansion velocity (derived from the cross section size of the CME flux rope) changes with distance, and (3) how the angular width (derived from footpoint separation) changes with distance. We further develop a time-dependent theoretical flux rope model to explain the observed kinematic and morphological evolution of CMEs. The model result can be used to constrain a number of important physical parameters in the interplanetary space, including solar wind aerodynamic dragging coefficient, magnetic dragging and plasma polytropic index.

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