Magnetohydrodynamic modeling of solar coronal dynamics with an initial non-force-free magnetic field

Abstract

The magnetic fields in the solar corona are generally neither force-free nor axisymmetric and have complex dynamics that are difficult to characterize. Here we simulate the topological evolution of solar coronal magnetic field lines (MFLs) using a magnetohydrodynamic model. The simulation is initialized with a non-axisymmetric non-force-free magnetic field that best correlates with the observed vector magnetograms of solar active regions (ARs). To focus on these ideas, simulations are performed for the flaring AR 11283 noted for its complexity and well-documented dynamics. The simulated dynamics develops as the initial Lorentz force pushes the plasma and facilitates successive magnetic reconnections at the two X-type null lines present in the initial field. Importantly, the simulation allows for the spontaneous development of mass flow, unique among contemporary works, that preferentially reconnects field lines at one of the X-type null lines. Consequently, a flux rope consisting of low-lying twisted MFLs, which approximately traces the major polarity inversion line, undergoes an asymmetric monotonic rise. The rise is attributed to a reduction in the magnetic tension force at the region overlying the rope, resulting from the reconnection. A monotonic rise of the rope is in conformity with the standard scenario of flares. Importantly, the simulated dynamics leads to bifurcations of the flux rope, which, being akin to the observed filament bifurcation in AR 11283, establishes the appropriateness of the initial field in describing ARs.

arXiv comment25 pages, 11 figures, published in The Astrophysical Journal

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Cited by in corpus (12)

• Magnetohydrodynamic Simulation of Magnetic Null-point Reconnections and Coronal dimmings during the X2.1 flare in NOAA AR 11283
• Magnetohydrodynamic simulation of magnetic null-point reconnections in NOAA AR12192 initiated with an extrapolated non-force-free-field
• An Eruptive Circular-ribbon Flare with Extended Remote Brightenings
• Magnetic reconnections in the presence of three-dimensional magnetic nulls and quasi-separatrix layers
• Formation of an observed eruptive flux rope above the torus instability threshold through tether-cutting magnetic reconnection
• On the partial eruption of a bifurcated solar filament structure
• Comparison of the Hall Magnetohydrodynamics and Magnetohydrodynamics evolution of a flaring solar active region
• Evolution of three-dimensional coherent structures in Hall magnetohydrodynamics
• MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation
• Study of magnetic field topology of active region 12192 using an extrapolated non-force-free magnetic field
• Formation and rising phase of a flux rope through data-constrained simulations
• Magnetohydrodynamics simulation of magnetic flux rope formation in a quadrupolar magnetic field configuration