Physics – Plasma Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh43a1935r&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH43A-1935
Physics
Plasma Physics
[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7526] Solar Physics, Astrophysics, And Astronomy / Magnetic Reconnection, [7827] Space Plasma Physics / Kinetic And Mhd Theory
Scientific paper
In order to predict the effects of solar eruptive events on the Space Weather at the Earth one needs to trace the perturbation through the solar corona and inner heliosphere. The majority of global numerical models to accomplish this tracing reduce the plasma description to the MHD approximation. On the other hand, the physics of solar eruptive events goes beyond the MHD formalism should we wish to quantify the rate of magnetic reconnection, the particle acceleration, as well as the wave-particle interaction. Studying these processes requires a kinetic plasma model. In this paper, we present a new global simulation tool that couples an MHD model and a Particle-In-Cell (PIC) numerical model. The MHD model combines a realistic three-dimensional MHD global model of the solar corona and inner heliosphere. The PIC model provides better local description of the physics associated with flare regions in the corona. This paper discusses the CME-flare physics associated with the model of Roussev et al. (2003) from two different perspectives: ideal MHD everywhere versus global MHD with local kinetic effects in current sheets. We compare the differences in the reconnection rates and the associated differences in magnetic field geometry and height-time profiles of the CME.
Downs Cooper
Gombosi Tamas I.
Roussev Ilia I.
Sokolov Iu. I.
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