A formation mechanism for the large plumes in the prominence
arXiv:2202.08521 · doi:10.1051/0004-6361/202142584
Abstract
To understand the formation mechanism of large plumes in solar prominences, we investigate the formation process of two such phenomena. We studied the dynamic and thermal properties of two large plumes using observations from New Vacuum Solar Telescope, the Solar Dynamic Observatory, and the Solar Terrestrial Relations Observatory-Ahead. We find that two large plumes observed with high-resolution data are quite different from previously studied small-scale plumes. They are born at the top of a prominence bubble with a large projected area of 10-20 Mm^2 . Before the occurrence of each large plume, the bubble expands and takes on a quasi-semicircular appearance. Meanwhile, the emission intensity of extreme-ultra-violet (EUV) bands increases in the bubble. A small-scale filament is found to erupt in the bubble during the second large plume. At the point at which the height of the bubble is comparable with half the width of the bubble, the bubble becomes unstable and generates the plumes. During the formation of plumes, two side edges of the top of the bubble, which are dominated by opposite Doppler signals, approach each other. The large plume then emerges and keeps rising up with a constant speed of about 13-15 km/s. These two large plumes have temperatures of 1.3 x 10^6 Kelvin and densities of 2.0 x 10^9 cm^-3, two orders hotter and one order less dense than the typical prominence. We also find that the bubble is a hot, low-density volume instead of a void region beneath the cold and dense prominence. Therefore, we conclude that these two large plumes are the result of the breakup of the prominence bubble triggered by an enhancement of thermal pressure; they separate from the bubble, most likely by magnetic reconnection.
arXiv comment14 pages, 7 figures, accepted for publication in A&A
References in corpus (18)
- Physics of Solar Prominences: II - Magnetic Structure and Dynamics
- Differential Emission Measures from the Regularized Inversion of Hinode and SDO data
- Thermal Diagnostics with the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory: A Validated Method for Differential Emission Measure Inversions
- Representations of world coordinates in FITS
- Generation of Solar Spicules and Subsequent Atmospheric Heating
- Velocity vectors of a quiescent prominence observed by Hinode/SOT and the MSDP (Meudon)
- Some interesting topics provoked by the solar filament research in the past decade
- The Temperature and Density Structure of the Solar Corona. I. Observations of the Quiet Sun with the EUV Imaging Spectrometer (EIS) on Hinode
- New Vacuum Solar Telescope observations of a flux rope tracked by a filament activation
- Numerical Simulations of the Magnetic Rayleigh-Taylor Instability in the Kippenhahn-Schlüter Prominence Model
- 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
- Two Kinds of Dynamic Behavior in a Quiescent Prominence Observed by the NVST
- Characterising motion types of G-band bright points in the quiet Sun
- Fine-scale structures and material flows of quiescent filaments observed by New Vacuum Solar Telescope
- Determination of Prominence Plasma Beta from the Dynamics of Rising Plumes
- EUV lines observed with EIS/Hinode in a solar prominence
- Mass motion in a prominence bubble revealing a kinked flux rope configuration
- Reconstructing 3D Magnetic Topology of On-disk Prominence Bubbles from Stereoscopic Observations