The Evolution of Magnetic Rayleigh-Taylor Unstable Plumes and Hybrid KH-RT Instability into A Loop-like Eruptive Prominence

Abstract

MRT unstable plumes are observed in a loop-like eruptive prominence using SDO/AIA observations. The small-scale cavities are developed within the prominence, where perturbations trigger dark plumes (P1 \& P2) propagating with the speed of 35-46 km s${}^{-1}$. The self-similar plume formation shows initially the growth of linear MRT unstable plume (P1), and thereafter the evolution of non-linear single mode MRT unstable second plume (P2). The Differential Emission Measure (DEM) analysis shows that plumes are less denser and hotter than the prominence. We have estimated the observational growth rate for both plumes as 1.32$\pm$0.29$\times$ 10${}^{-3}$ s${}^{-1}$ and 1.48$\pm$0.29$\times$ 10${}^{-3}$ s${}^{-1}$ respectively, which are comparable to the estimated theoretical growth rate (1.95$\times$ 10${}^{-3}$ s${}^{-1}$) . The nonlinear phase of an MRT unstable plume (P2) may collapse via Kelvin-Helmholtz vortex formation in the downfalling plasma. Later, a plasma thread has been evident in the rising segment of this prominence. It may be associated with the tangled field and Rayleigh-Taylor instability. The tangled field initiates shearing at the prominence-cavity boundary. Due to this shear motion, the plasma downfall has occurred at the right part of the prominence-cavity boundary. It triggers the characteristic of KH unstable vortices and MRT unstable plasma bubbles propagating at different speeds and merging with each other. The shear motion and lateral plasma downfall may initiate hybrid KH-RT instability there.

arXiv comment25 pages, 8 figures, 1 table

References in corpus (19)

• Physics of Solar Prominences: I - Spectral Diagnostics and Non-LTE Modelling
• Thermal Diagnostics with the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory: A Validated Method for Differential Emission Measure Inversions
• Differential Emission Measure Analysis of Multiple Structural Components of Coronal Mass Ejections in the Inner Corona
• Multi-scale Gaussian normalization for solar image processing
• The Magnetic Rayleigh-Taylor Instability in Three Dimensions
• SDO/AIA Observation of Kelvin-Helmholtz Instability in the Solar Corona
• Investigation of the Formation and Separation of An EUV Wave from the Expansion of A Coronal Mass Ejection
• Velocity vectors of a quiescent prominence observed by Hinode/SOT and the MSDP (Meudon)
• The discovery of geomagnetically trapped cosmic ray antiprotons
• Break up of returning plasma after the 7 June 2011 filament eruption by Rayleigh-Taylor instabilities
• Tangled Magnetic Fields in Solar Prominences
• Numerical Simulations of the Magnetic Rayleigh-Taylor Instability in the Kippenhahn-Schlüter Prominence Model
• Flux cancellation and the evolution of the eruptive filament of 2011 June 7
• Investigating the Dynamics and Density Evolution of Returning Plasma Blobs from the 2011 June 7 Eruption
• 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
• Rayleigh-Taylor instabilities with sheared magnetic fields
• Evolution of Magnetic Rayleigh-Taylor Instability into the Outer Solar Corona and Low Inter Planetary Space
• Observations of Plasma Blob Ejection from a Quiescent Prominence by Hinode SOT
• Flows and Waves in Braided Solar Coronal Magnetic Structures

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• Reconstructing 3D Magnetic Topology of On-disk Prominence Bubbles from Stereoscopic Observations
• Magnetic Rayleigh-Taylor Instability at a Contact Discontinuity With Oblique Magnetic Field
• Simulating Rayleigh-Taylor induced magnetohydrodynamic turbulence in prominences
• Evolution of Kelvin-Helmholtz Instability in the Fan-Spine Topology
• The prominence driven forced reconnection in the solar corona and associated plasma dynamics