Abstract

The magnetic Rayleigh–Taylor instability is a fundamental instability of many astrophysical systems, and recent observations are consistent with this instability developing in solar prominences. Prominences are cool, dense clouds of plasma that form in the solar corona that display a wide range of dynamics of a multitude of spatial and temporal scales, and two different phenomena that have been discovered to occur in prominences can be understood as resulting from the Rayleigh–Taylor instability. The first is that of plumes that rise through quiescent prominences from low density bubbles that form below them. The second is that of a prominence eruption that fragments as the material falls back to the solar surface. To identify these events as the magnetic Rayleigh–Taylor instability, a wide range of theoretical work, both numerical and analytical has been performed, though alternative explanations do exist. For both of these sets of observations, determining that they are created by the magnetic Rayleigh–Taylor instability has meant that the linear instability conditions and nonlinear dynamics can be used to make estimates of the magnetic field strength. There are strong connections between these phenomena and those in a number of other astro, space and plasma systems, making these observations very important for our understanding of the role of the Rayleigh–Taylor instability in magnetised systems.

Highlights

  • The topic of this review paper is the magnetic Rayleigh–Taylor instability in solar prominences

  • To identify these events as the magnetic Rayleigh–Taylor instability, a wide range of theoretical work, both numerical and analytical has been performed, though alternative explanations do exist. For both of these sets of observations, determining that they are created by the magnetic Rayleigh–Taylor instability has meant that the linear instability conditions and nonlinear dynamics can be used to make estimates of the magnetic field strength

  • There is the observation of a prominence eruption observed by the atmospheric imaging assembly (AIA: Lemen et al 2012) onboard the Solar Dynamics Observatory (SDO) that fragments as it falls back towards the solar surface in a way that is strongly reminiscent of water splashes and milk crowns

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Summary

Introduction

The topic of this review paper is the magnetic Rayleigh–Taylor instability in solar prominences. There is the observation of a prominence eruption observed by the atmospheric imaging assembly (AIA: Lemen et al 2012) onboard the Solar Dynamics Observatory (SDO) that fragments as it falls back towards the solar surface in a way that is strongly reminiscent of water splashes and milk crowns These observations of the Rayleigh–Taylor instability are, in the authors somewhat biased opinion, the best examples that exist in astrophysics. I will present information gleaned from observations of prominence dynamics and present the theoretical work that connects these observations to the magnetic Rayleigh–Taylor instability At this point, I will look at the other explanations that have been put forward to explain this phenomenon. I will connect between these observations and other astrophysical, space and plasma systems

Prominences
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Prominence models
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G 10À13 q g
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Dynamics of prominences
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Prominence plumes
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Prominence bubbles
30 Bubble
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Fragmenting eruption
The magnetic Rayleigh–Taylor instability
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Theoretical interpretation of the observations
The Rayleigh–Taylor instability
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Local simulations of prominence plumes
Simulating this instability in a global prominence model
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Kelvin–Helmholtz modes
Other buoyancy modes
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Comparison between models
Fragmenting eruption and the magnetic Rayleigh–Taylor
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Linear growth rate of the RT instability
Nonlinear plume flows
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The solar atmosphere and the heliosphere
Plasma and fluid experiments
Astrophysical systems
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Summary
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Compliance with ethical standards
Findings
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Full Text
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