Propagation of Coronal Mass Ejections in 3D and the Structure of the Inner Heliosphere

Details Propagation of Coronal Mass Ejections in 3D and the Structure of the Inner Heliosphere Propagation of Coronal Mass Ejections in 3D and the Structure of the Inner Heliosphere

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh34c..02g&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH34C-02

Astronomy and Astrophysics

Astrophysics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections

Scientific paper

Solar coronal mass ejections (CMEs) are the most significant drivers of adverse space weather on Earth, but the physics governing their propagation through the heliosphere is not well understood. Although stereoscopic imaging of CMEs with NASA's Solar Terrestrial Relations Observatory (STEREO) has provided some insight into their three-dimensional (3D) propagation, the mechanisms governing their evolution remain unclear because of difficulties in reconstructing their true 3D structure. In this talk I will describe the use of an elliptical tie-pointing technique to reconstruct a CME front in 3D, enabling us to quantify its deflected trajectory from high latitudes along the ecliptic, and measure its increasing angular width and propagation. At large distances from the Sun (>7 R_sun), I will describe how its motion is determined by drag effects in the solar wind, using ENLIL simulations of the inner heliosphere. By combining a 3D reconstruction with modelling of the solar wind, we predict an arrival time within 30 mins of the in-situ detection of the CME at ACE

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