Validation of a New Method to Derive Sun-to-1 AU Kinematics of ICMEs with a Numerical Simulation

Details Validation of a New Method to Derive Sun-to-1 AU Kinematics of ICMEs with a Numerical Simulation Validation of a New Method to Derive Sun-to-1 AU Kinematics of ICMEs with a Numerical Simulation

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh23c1970r&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH23C-1970

Astronomy and Astrophysics

Astrophysics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7959] Space Weather / Models

Scientific paper

The Heliospheric Imagers (HI) aboard the NASA STEREO mission offer the possibility to follow coronal mass ejections (CMEs) continuously on their way from close to the Sun up to ~ 1 AU. The interpretation of these images is challenging because line-of-sight as well as Thomson scattering effects influence the white-light signal. There are different methods to derive the velocity profiles and propagation directions of CMEs in the interplanetary space, e.g. Fixed-Φ (Kahler and Webb, 2007) and Harmonic Mean (Lugaz, Vourlidas and Roussev, 2009), which make the assumptions of a point like structure and a circle shaped front of the CME, respectively. These two approaches can be constrained using in situ measurements at 1 AU as shown in Rollett et al. (2011). To validate the applied methods, we perform the same procedures for a simulated CME as modeled in the space weather modeling framework (SWMF, Toth, et al., 2005). The measurements are outlined for synthetic HI images (Lugaz et al., 2005) at different observing points. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 263252 [COMESEP].

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