Downstream structure and evolution of a simulated CME-driven sheath in the solar corona

Details Downstream structure and evolution of a simulated CME-driven sheath in the solar corona Downstream structure and evolution of a simulated CME-driven sheath in the solar corona

Mar 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011a%26a...527a..46l&link_type=abstract

Astronomy & Astrophysics, Volume 527, id.A46

Astronomy and Astrophysics

Astrophysics

1

Magnetohydrodynamics (Mhd), Magnetic Fields, Sun: Coronal Mass Ejections (Cmes)

Scientific paper

Context. The transition of the magnetic field from the ambient magnetic field to the ejecta in the sheath downstream of a coronal mass ejection (CME) driven shock is analyzed in detail. The field rotation in the sheath occurs in a two-layer structure. In the first layer, layer 1, the magnetic field rotates in the coplanarity plane (plane of shock normal and the upstream magnetic field), and in layer 2 rotates off this plane. We investigate the evolution of the two layers as the sheath evolves away from the Sun. Aims: In situ observations have shown that the magnetic field in the sheath region in front of an interplanetary coronal mass ejection (ICME) form a planar magnetic structure, and the magnetic field lines drape around the flux tube. Our objective is to investigate the magnetic configuration of the CME near the sun. Methods: We used the space weather modeling framework (SWMF), a 3D magnetohydrodynamics (MHD) simulation code, to simulate the propagation of CMEs and the shock driven by it. Results: We find that close to the Sun, layer 2 dominates the width of the sheath, diminishing its importance as the sheath evolves away from the Sun, in agreement with observations at 1 AU.

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