Connecting CME expansion from Sun to 1 AU

Details Connecting CME expansion from Sun to 1 AU Connecting CME expansion from Sun to 1 AU

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh23b1841n&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH23B-1841

Astronomy and Astrophysics

Astrophysics

[2101] Interplanetary Physics / Coronal Mass Ejections, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections

Scientific paper

EUV disk imagers and white light coronagraphs have provided for many years information on the early formation and evolution of coronal mass ejections (CMEs). More recently, the novel heliospheric imaging instruments aboard the STEREO mission are providing crucial remote sensing information on the interplanetary evolution of these events while in situ instruments complete the overall characterization of the interplanetary CMEs. In this work, we present an analysis of CMEs from the Sun to the interplanetary medium using combined data from SDO, SOHO, STEREO, WIND, and ACE spacecraft. From the remote sensing analysis, the most notable feature of a CME observed in the SECCHI suite of instruments field of view is its elliptic cross section. However, most of the models for in situ modeling impose the circular cross-section geometry. In this work, we link the remote sensing observations with the in situ data through an analytical in situ model which incorporates the distortion in the cross-section. In this study, different aspects such as the ambient solar wind, magnetic field configurations, plasma parameters, etc, have been taken into account in order to cover the widest spectrum of possible scenarios.

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