Interlocked MHD modeling of the Launching and Propagation of Coronal Mass Ejections

Details Interlocked MHD modeling of the Launching and Propagation of Coronal Mass Ejections Interlocked MHD modeling of the Launching and Propagation of Coronal Mass Ejections

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsm41a0312s&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SM41A-0312

Physics

7509 Corona, 7513 Coronal Mass Ejections (2101), 7519 Flares, 7524 Magnetic Fields, 7959 Models

Scientific paper

Coronal mass ejections (CMEs) are not only one of the most energetic phenomena in the solar corona but also a key process in the space weather study. The numerical modeling of the launching and propagation of CMEs play a crucial role for space weather forecast. However, due to the vast difference in the spatial scale among solar, solar wind, and terrestrial plasmas, it is difficult and wasteful of numerical resource to simulate the whole process associated with the initiation and propagation of CMEs with a single simulation model. Therefore, we have recently developed a new numerical model, which can continuously calculate the whole process from the onset of CMEs to the geomagnetic impact of that, using the interlocking of several numerical models. The model consists of four numerical models; the solar active region model, the global corona model, the interplanetary space model, and the geospace model. In this paper, we explain the basic algorithm of the interlocked modeling, and show some important results obtained with it. First, we investigate the physical relationship between the solar magnetic field structure and the launching of CMEs. CMEs are ejections of a large amount of mass and magnetic flux, which result from eruptions of coronal magnetic field. Although the eruptions may cause solar flares, many observations show that all flares are not necessarily associated with CMEs, implying that there are some kinds of criteria. For example, it is likely that an eruption is confined by the ambient global magnetic field if the eruption is not large enough or if its direction of magnetic field is not appropriate. In order to examine the condition whether the eruption of coronal field can be launched as a CME, we performed a three-dimensional MHD simulation of an eruption in various global coronal magnetic fields, and succeeded to distinguish the condition capable of a CME. For example, an eruption of a small and strong magnetic field active region cannot be ejected as a CME due to magnetic tension force of anchored field. In this paper, we summarize the relationship between the key parameters for the ejection; the amount of magnetic flux and field directions. Second, our interlocked model is applied onto the CME event caused by the X-class flare occurring on the active region NOAA 10930 on December 13, 2006. The numerical experiment is initiated by the magnetic field model, which is constructed based on the magnetogram data observed by the Solar Optical Telescope (SOT) boarded on Hinode satellite, and the simulated variation of magnetic field and plasma state at the Earth orbit is compared with the in-situ observation by ACE. As a result, it is found that a relatively good agreement can be obtained between the simulation and observation if we parameterize the magnetic field on the CME launching site.

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