Document Type

Journal Article

Journal Article Version

Final Version / Publisher's PDF (peer-reviewed)

Publication Date

9-1-2010

Abstract

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 paper, we use a new elliptical tie-pointing technique to reconstruct a full 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 from 2 to 46 R-circle dot (similar to 0.2 AU). Beyond 7 R-circle dot, we show that its motion is determined by an aerodynamic drag in the solar wind and, using our reconstruction as input for a 3D magnetohydrodynamic simulation, we determine an accurate arrival time at the Lagrangian L1 point near Earth.

Published in

Nature Communications

DOI

10.1038/ncomms1077

Keywords

Sun: coronal mass ejections (CMEs), heliosphere, Space weather

Department / Organizational Unit

Astronomy

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