A Multi-vantage Point Study Of A CME Event Using SOHO/LASCO And STEREO Observations Together With The WSA/ENLIL Solar Wind And Cone CME Model

Details A Multi-vantage Point Study Of A CME Event Using SOHO/LASCO And STEREO Observations Together With The WSA/ENLIL Solar Wind And Cone CME Model A Multi-vantage Point Study Of A CME Event Using SOHO/LASCO And STEREO Observations Together With The WSA/ENLIL Solar Wind And Cone CME Model

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.2308l&link_type=abstract

American Astronomical Society, SPD meeting #42, #23.08; Bulletin of the American Astronomical Society, Vol. 43, 2011

Physics

Scientific paper

As we progress toward the maximum period of Solar Cycle 24, we have a unique opportunity to better understand the propagation and evolution of a CME given the multiple vantage points near 1 AU of such an event. In addition, with the wide availability of sophisticated, physics-based solar wind models, we can obtain a more global view of the CME evolution and propagation through numerical simulations. In this study, we simulate a CME event using the WSA/ENLIL 3D MHD solar wind model and daily updated solar magnetograms from GONG. To characterize the CME in the model, we use a simple geometrical description that assumes a cone shape for a CME and determine the CME width and central position from white light coronagraph images. We select a CME event that is observed by both STEREO (A and/or B) and SOHO/LASCO. Currently, both STEREO spacecraft are located 90 degrees away from LASCO at L1. For a CME directed toward L1, i.e., a `halo event', the same CME is observed as a limb event by STEREO. Such limb observations are ideal for determining the initial CME speed and width since there are less plane-of-sky projection effects. From a space weather perspective, studying halo CME events is important since they can strongly affect the space environment near Earth. To assess the accuracy of the cone+WSA/ENLIL model and the self-consistency of the results at different `vantage points’ in the model, we compare the modeled solar wind density, speed, and magnetic field magnitude with the values measured in-situ by ACE at L1 and STEREO.

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