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Paper: Simulations of the Dynamics of the Magnetic Rayleigh–Taylor Instability in Solar Prominences
Volume: 474, Numerical Modeling of Space Plasma Flows (ASTRONUM2012)
Page: 147
Authors: Hillier, A.; Berger, T.; Shibata, K.; Isobe, H.
Abstract: The magnetic Rayleigh–Taylor instability plays an important role in the mass and magnetic flux transport in many astrophysical bodies. Solar prominences also display this instability and recent observations using the Solar Optical Telescope onboard the Hinode satellite have revealed these dynamics in amazing detail. The observations show rising plumes, approximately 1 Mm in width, that propagate through the dense prominence material from low-density bubbles, i.e. the situation expected when the magnetic Rayleigh–Taylor instability occurs. To study this phenomenon, we performed 3D simulations of the magnetic Rayleigh–Taylor instability in the Kippenhahn–Schlüter prominence model. The plumes formed in these simulations are filamentary structures that are aligned with the magnetic field created as 3D modes of the magnetic Rayleigh–Taylor instability. The plumes rise, developing large structures from smaller structures through an inverse cascade process driven by nonlinear interaction. The results suggest that the plumes observed in the prominence may be used to study the conditions inside the prominence.
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