Imaging Coronal Mass Ejections and Large-Scale Solar Wind Structure Using Thomson-Scattering Measurements from SMEI

Details Imaging Coronal Mass Ejections and Large-Scale Solar Wind Structure Using Thomson-Scattering Measurements from SMEI Imaging Coronal Mass Ejections and Large-Scale Solar Wind Structure Using Thomson-Scattering Measurements from SMEI

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh21a1909j&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH21A-1909

Astronomy and Astrophysics

Astrophysics

[2101] Interplanetary Physics / Coronal Mass Ejections, [2111] Interplanetary Physics / Ejecta, Driver Gases, And Magnetic Clouds, [2194] Interplanetary Physics / Instruments And Techniques, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections

Scientific paper

In January 2010, two coronal mass ejections (CMEs) erupted from near the solar east limb, the first on late 14 January 2010 and the second on 17 January 2010. Both arrived at the Solar TErrestrial RElations Observatory Behind spacecraft (STEREO-B) about six days later. We are able to reconstruct the heliospheric density of both CME events in three dimensions (3D) using data from the Solar Mass Ejection Imager (SMEI) and our tomographic analysis. For each event, we isolate the particular portion of the heliosphere attributed to the transient CME density structure from the tomographic results, and then estimate its extent. The structure of these events is shown in detail in the three-dimensional reconstruction both as pseudo-coronagraph images and later as density at the locations of STEREO-B and the Earth. The first of these CMEs was associated with a magnetic cloud that had a density enhancement near its center. By assuming that this density enhancement extends along the loop, we can use the three-dimensional density analysis to map the extent and orientation of this structure in order to match it to existing magnetic-loop models and to use the remote-sensing observations to constrain the various flux-rope models determined using the in-situ measurements of the 14 January 2010 event.

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