Solar prominences: 'double, double ... boil and bubble'
arXiv:1505.05268 · doi:10.1088/2041-8205/806/1/L13
Abstract
Observations revealed rich dynamics within prominences, the cool 10,000 K, macroscopic (sizes of order 100 Mm) "clouds" in the million degree solar corona. Even quiescent prominences are continuously perturbed by hot, rising bubbles. Since prominence matter is hundredfold denser than coronal plasma, this bubbling is related to Rayleigh-Taylor instabilities. Here we report on true macroscopic simulations well into this bubbling phase, adopting a magnetohydrodynamic description from chromospheric layers up to 30 Mm height. Our virtual prominences rapidly establish fully non-linear (magneto)convective motions where hot bubbles interplay with falling pillars, with dynamical details including upwelling pillars forming within bubbles. Our simulations show impacting Rayleigh-Taylor fingers reflecting on transition region plasma, ensuring that cool, dense chromospheric material gets mixed with prominence matter up to very large heights. This offers an explanation for the return mass cycle mystery for prominence material. Synthetic views at extreme ultraviolet wavelengths show remarkable agreement with observations, with clear indications of shear-flow induced fragmentations.
arXiv comment18 pages, 5 figures
References in corpus (12)
- MPI-AMRVAC for Solar and Astrophysics
- Accretion to Magnetized Stars through the Rayleigh-Taylor Instability: Global Three-Dimensional Simulations
- Simulations of Prominence Formation in the Magnetized Solar Corona by Chromospheric Heating
- Formation of Solar Filaments by Steady and Nonsteady Chromospheric Heating
- Simulating the in situ condensation process of solar prominences
- Rayleigh-Taylor instability in Magnetohydrodynamic Simulations of the Crab Nebula
- Multidimensional modeling of coronal rain dynamics
- Rayleigh-Taylor instability in prominences from numerical simulations including partial ionization effects
- Morphology and dynamics of solar prominences from 3D MHD simulations
- Numerical Simulations of the Magnetic Rayleigh-Taylor Instability in the Kippenhahn-Schlüter Prominence Model
- The Dynamics of Funnel Prominences
- Rayleigh-Taylor instabilities with sheared magnetic fields
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- Quiescent prominence dynamics observed with the Hinode Solar Optical Telescope . II. Prominence Bubble Boundary Layer Characteristics and the Onset of a Coupled Kelvin-Helmholtz Rayleigh-Taylor Instability
- Coronal rain in magnetic bipolar weak fields
- Prominence formation by levitation-condensation at extreme resolutions
- On the nature of the magnetic Rayleigh-Taylor instability in Astrophysical Plasma: The case of uniform magnetic field strength
- Particle acceleration by magnetic Rayleigh-Taylor instability: mechanism for flares in black-hole accretion flows
- Sympathetic Filament Eruptions within a Fan-spine Magnetic System
- Impact of Dynamic State on the Mass Condensation Rate of Solar Prominences
- Magnetic field amplification and structure formation by the Rayleigh-Taylor instability
- Reconfiguration and eruption of a solar filament by magnetic reconnection with an emerging magnetic field
- Dynamics of descending knots in a solar prominence and their possible contributions to the heating of the local corona
- Simulating Rayleigh-Taylor induced magnetohydrodynamic turbulence in prominences
- Fast Sausage Oscillations in Coronal Loops with Fine Structures