Two Kinds of Dynamic Behavior in a Quiescent Prominence Observed by the NVST
| Autor: | Qingmin Zhang, Yuandeng Shen, Tuanhui Zhou, Zongjun Ning, Dong Li |
|---|---|
| Rok vydání: | 2018 |
| Předmět: |
Physics
010504 meteorology & atmospheric sciences Deformation (mechanics) FOS: Physical sciences Astronomy and Astrophysics Mechanics Plasma 01 natural sciences Instability Solar prominence Shear (sheet metal) Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science 0103 physical sciences Physics::Space Physics Supersonic speed Clockwise Magnetohydrodynamic drive 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) 0105 earth and related environmental sciences |
| DOI: | 10.48550/arxiv.1807.03942 |
| Popis: | We present high-resolution observations of two kinds of dynamic behavior in a quiescent prominence using the New Vacuum Solar Telescope, i.e., Kelvin-Helmholtz instabilities (KHIs) and small-scale oscillations. The KHIs were identified as rapidly developed vortex-like structures with counter-clockwise/clockwise rotations in the Ha red-wing images at +0.3 A, which were produced by the strong shear-flows motions on the surface/interface of prominence plumes. The KHI growth rates are estimated to be about 0.0135 +(-)0.0004 and 0.0138 +(-) 0.0004. Our observational results further suggest that the shear velocities (i.e, supersonic) of the mass flows are fast enough to produce the strong deformation of the boundary and overcome the restraining surface tension force. This flow-driven instability might play a significant role in the process of plasma transfer in solar prominences. The small-scale oscillations perpendicular to the prominence threads are observed in the Ha line-center images. The oscillatory periods changed non-monotonically and showed two changing patterns, in which one firstly decreased slowly and then it changed to increase, while the other grew fast at the beginning and then it changed to decrease. Both of these two thread oscillations with changing periods were observed to be unstable for an entire cycle, and they were local in nature. All our findings indicate that the small-scale thread oscillations could be magnetohydrodynamic waves in the solar corona. Comment: 22 pages, 8 figures, 1 table, accepted for publication in The Astrophysical Journal |
| Databáze: | OpenAIRE |
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