Filamentary structure on the Sun from the magnetic Rayleigh–Taylor instability

Hiroaki Isobe (), Takehiro Miyagoshi, Kazunari Shibata and Takaaki Yokoyama
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Hiroaki Isobe: Kyoto University
Takehiro Miyagoshi: Kyoto University
Kazunari Shibata: Kyoto University
Takaaki Yokoyama: University of Tokyo

Nature, 2005, vol. 434, issue 7032, 478-481

Abstract: Corona heated by lighter fluid Among the structures observed on the Sun's surface are dark filaments connecting sunspots of opposite polarity. These are associated with the emergence of magnetic flux from the Sun's interior, and their jet activity and X-ray emission suggest a role in coronal heating. In the first astrophysics calculations performed on the Earth Simulator, a supercomputer with possibly the highest simulation performance in the world, filamentary structures are shown to arise spontaneously from Rayleigh–Taylor instability, an instability that occurs when a dense heavy fluid is accelerated by a light fluid. This can account for the intermittence of coronal heating and patchy brightening of solar flares.

Date: 2005
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DOI: 10.1038/nature03399

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