Evolution of Piled-up Compressions in Modeled Coronal Mass Ejection Sheaths and the Resulting Sheath Structures

Details Evolution of Piled-up Compressions in Modeled Coronal Mass Ejection Sheaths and the Resulting Sheath Structures Evolution of Piled-up Compressions in Modeled Coronal Mass Ejection Sheaths and the Resulting Sheath Structures

Mar 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011apj...729..112d&link_type=abstract

The Astrophysical Journal, Volume 729, Issue 2, article id. 112 (2011).

Astronomy and Astrophysics

Astronomy

3

Magnetohydrodynamics: Mhd, Sun: Corona, Sun: Coronal Mass Ejections: Cmes

Scientific paper

We study coronal mass ejection (CME)-driven shocks and the resulting post-shock structures in the lower corona (2-7 R sun). Two CMEs are erupted by modified Titov-Démoulin (TD) and Gibson-Low (GL) type flux ropes (FRs) with the 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/FR moves and expands in the solar wind medium, it pushes the magnetized material lying 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 is 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 is 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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