Y. C.-M. Liu, M. Opher, O. Cohen P.C.Liewer and T.I.Gombosi

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Presentation transcript:

Y. C.-M. Liu, M. Opher, O. Cohen P.C.Liewer and T.I.Gombosi A Simulation of a CME Propagation and Shock Evolution in the Lower Solar Corona Y. C.-M. Liu, M. Opher, O. Cohen P.C.Liewer and T.I.Gombosi George Mason University 01/03/2007

Outline CME and Solar Energetic Particles Why Lower Solar corona? Space Weather Modeling Framework Brief Introduction Simulations Background Solar Wind Initiate a CME Results Shock evolution, CME dynamics Conclusions

CME and SEPs Stereo Modified from Lee, 2005

Space Weather Modeling Framework Inner Heliosphere (IH) Solar Corona (SC) 24 Rs 1AU Rs is solar radii

MHD Equations

Heating?- Parameterized by 

The Solar Wind CR 1922 solar minimum CR1922

CME Initiation Loss of equilibrium! The magnetic field under study is modeled by a force-free circular flux tube with the total current I, a pair of magnetic charges q and a line current I0. Below the photospheric plane. The flux tube is at force balance. Titov and Demoulin 1999

The inserted TD flux rope

Rising Flux Rope

Bright Front and Dark Void 2D slice at Z=0.11 t=10 minutes

Shock Speed and the background solar wind speed

Why Acceleration? The acceleration determined by F=Ma CME Pressures Drag Force Fd Gravity Sun The acceleration determined by F=Ma M=Mass_CME + Virtual Mass Fd=V2 Cd Forbes et al, 2006

The Density Peak after the Shock

Predicted and Modeled Acceleration 1 Cd=1, Mv=0; 2. Cd=tanhß, Mv=0; 3. Cd=1, considering Mv 4. Cd=tanhß, considering Mv, 5. Modeled acceleration

The Forces

Shock and Post Shock Compression Ratio

New Progress Forbes 1995?

More at: http://physics.gmu.edu/~yliuc/SWMF_Result _MAY14_2007/PostAGU2007/2Dslices/2D_slice_MagneticEvolution.html

Summary and Conclusions We present the first detailed CME simulation in the lower solar corona using SWMF Shock is nearly perpendicular at the nose The acceleration of the CME is controlled by the pressure forces and the drag force. Magnetic pressure contributes to the acceleration at the bottom of the solar corona The post shock acceleration exists in 3-5 Rs and it could contribute to the particle acceleration The configuration near the sheath needs to be resolved.