End-to-End Observations and Modeling of the 17-21 January 2010 CME/ICME

Details End-to-End Observations and Modeling of the 17-21 January 2010 CME/ICME End-to-End Observations and Modeling of the 17-21 January 2010 CME/ICME

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh41a1778w&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH41A-1778

Astronomy and Astrophysics

Astrophysics

[2101] Interplanetary Physics / Coronal Mass Ejections, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7974] Space Weather / Solar Effects

Scientific paper

On 17 January 2010, before it rotated onto the Earth-facing disk and produced a series of M-class X-ray flares, active region 11041 was associated with an energetic CME with a coronal wave and dimming, radio type II and III emission. During launch the CME revealed an unusual circular profile viewed from STEREO-B with EUVI and extending into the COR1 field. It was also observed over the southeast limb from SOHO EIT and LASCO from which it appeared as a partial halo. The views from STEREO and SOHO near the Sun and HI-A and SMEI at 1 AU suggest that at least part of the CME traveled toward STEREO-B, where a small magnetic cloud was observed on 21 January. The importance of this event lies in the multiwavelength observations with high time cadences of near-limb observations of a CME, its manifestations in the low corona, its passage through the heliosphere and its appearance as an ICME/magnetic cloud in-situ at STEREO-B 3.5 days later. This event permits us to study the origin and driving of the wave because the flanks of the CME and its relationship to the wave can be studied in detail. Our interpretation is that the wave is initially driven by the CME and then becomes freely propagating after the CME lateral expansion ends. Several models are used to understand the 3-D geometry and propagation of the CME, and two flux rope models are compared with the launch observations and magnetic field orientations.

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