Evolution of Piled Up Compressions in Modeled CME Sheaths and the Resulting Sheath Structures

Details Evolution of Piled Up Compressions in Modeled CME Sheaths and the Resulting Sheath Structures Evolution of Piled Up Compressions in Modeled CME Sheaths and the Resulting Sheath Structures

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh51e1732d&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH51E-1732

Astronomy and Astrophysics

Astrophysics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections

Scientific paper

We study Coronal Mass Ejection (CME) driven shocks and the resulting post shock structures in the lower corona (~ 2-7 Rsun). Two CMEs are erupted by modified Titov-Demoulin (TD) and Gibson-Low (GL) type flux ropes with Space Weather Modeling Framework. We observe a substantial pile up of density compression and a narrow region of plasma depletion layer (PDL) in the simulations. As the CME/flux rope moves and expands in solar wind medium, it pushes the magnetized material laying ahead of it. Hence, the magnetic field lines draping around the CME front are compressed in the sheath just ahead of the CME. These compressed field lines squeeze out the plasma sideways forming PDL in the region. Solar plasma being pushed and displaced from behind, forms a strong piled up compression (PUC) of density downstream of the PDL. Both CMEs have comparable propagation speeds while GL has larger expansion speed than TD due to its higher initial magnetic pressure. We argue that high CME expansion speed along with high solar wind density in the region are responsible for the large PUC found in the lower corona. In case of GL the PUC is much wider although the density compression ratio for both the cases are comparable. Although these simulations artificially initiate out-of-equilibrium CMEs and drive them in an artificial solar wind solution, we predict that PUCs, in general, will be large in the lower corona. This should affect the ion profiles of the accelerated solar energetic particles.

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