MHD Modeling for Formation Process of Coronal Mass Ejections: Interaction between Ejecting Flux Rope and Ambient Field

Abstract

We performed magnetohydrodynamic simulation of a formation process of coronal mass ejections (CMEs), focusing on interaction (reconnection) between an ejecting flux rope and its ambient field. We examined three cases with different ambient fields: no ambient field, and cases with dipole field of two opposite directions which are parallel and anti-parallel to that of the flux rope surface. As a result, while the flux rope disappears in the anti-parallel case, in other cases the flux ropes can evolve to CMEs and show different amounts of rotation of the flux rope. The results imply that the interaction between an ejecting flux rope and its ambient field is an important process for determining CME formation and CME orientation, and also show that the amount and direction of magnetic flux within the flux rope and the ambient field are key parameters for CME formation. Especially, the interaction (reconnection) plays a significant role to the rotation of the flux rope, with a process similar to "tilting instability" in a spheromak-type experiment of laboratory plasma.

24 pages, 5 figures. Accepted for publication in ApJ

References in corpus (5)

• Torus instability
• Formation of current sheets and sigmoidal structure by the kink instability of a magnetic loop
• Eruption of magnetic flux ropes during flux emergence
• The effect of the relative orientation between the coronal field and new emerging flux: I Global Properties
• Relationship between EIT Post Eruption Arcades, Coronal Mass Ejections, Coronal Neutral Line and Magnetic Clouds

Cited by in corpus (18)

• Hydrodynamics of core-collapse supernovae and their progenitors
• Electric current in flares ribbons: observations and 3D standard model
• Quantitative Analysis of CME Deflections in the Corona
• Numerical Investigation of a Coronal Mass Ejection from an Anemone Active Region: Reconnection and Deflection of the 2005 August 22 Eruption
• Magnetic Flux Ropes in the Solar Corona: Structure and Evolution toward Eruption
• A Parametric Study of Erupting Flux Rope Rotation. Modeling the "Cartwheel CME" on 9 April 2008
• Magnetohydrodynamic Modeling of a Solar Eruption Associated with X9.3 Flare Observed in Active Region 12673
• Signatures of magnetic reconnection at boundaries of interplanetary small-scale magnetic flux ropes
• Unambiguous Evidence of Filament Splitting-Induced Partial Eruptions
• A Challenging Solar Eruptive Event of 18 November 2003 and the Causes of the 20 November Geomagnetic Superstorm. IV. Unusual Magnetic Cloud and Overall Scenario
• Self-consistent propagation of flux ropes in realistic coronal simulations
• The spheromak tilting and how it affects modelling coronal mass ejections
• A study of the Heliocentric dependence of Shock Standoff Distance and Geometry using 2.5D MHD Simulations of CME-driven shocks
• Eruption and propagation of twisted flux ropes from the base of the solar corona to 1 au
• APSARA: A multi-dimensional unsplit fourth-order explicit Eulerian hydrodynamics code for arbitrary curvilinear grids
• Influence of Earth-Directed Coronal Mass Ejections on the Sun's Shadow Observed by the Tibet-III Air Shower Array
• Formation and Eruption of Hot Channels during an M6.5 Class Solar Flare
• Helical Kink Instability in the confined Solar Eruption on 2002 May 27