Numerical Simulation of Interplanetary Coronal Mass Ejections and STEREO Observations

Details Numerical Simulation of Interplanetary Coronal Mass Ejections and STEREO Observations Numerical Simulation of Interplanetary Coronal Mass Ejections and STEREO Observations

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agusmsh22a..05o&link_type=abstract

American Geophysical Union, Spring Meeting 2009, abstract #SH22A-05

Physics

2101 Coronal Mass Ejections (7513), 2102 Corotating Streams, 2139 Interplanetary Shocks, 7924 Forecasting (2722), 7959 Models

Scientific paper

Since numerical simulation of solar eruptions is still in research phase various empirically-based techniques have been developed for predicting arrivals of coronal mass ejections (CMEs) at the Earth. These techniques take advantage of remote observations of CMEs in coronagraphs, fit their geometric and kinematic properties, and apply kinematic or numerical model to predict heliospheric propagation and evolution. Due to limited remote and in-situ observations, simple geometric structures have been assumed so far and the validation of such predictions has been limited. We use the 3-D numerical heliospheric code ENLIL to simulate propagation of well-observed interplanetary CMEs in 2007 and 2008. This heliospheric code uses the MAS or WSA coronal model for computing the structured background solar wind and the so-called CME cone model for specification of the geometric and kinematic parameters of the hydrodynamic transient disturbances. We use the ACE, MESSENGER, and STEREO in-situ observations to constrain the model predictions. We found that "traditional" approaches based on simple cone models over-predicts disturbances at those spacecraft. New geometric models of CMEs are clearly needed and we have incorporated rope-like hydrodynamic structure. We present result achieved by launching the cone-like and rope-like structures and compare the heliospheric predictions with the multi-spacecraft in-situ observations.

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