Multilayered Kelvin–Helmholtz Instability in the Solar Corona

Yuan, Ding; Shen, Yuandeng; Liu, Yu; Li, Hongbo; Feng, Xueshang; Keppens, Rony

doi:10.3847/2041-8213/ab4bcd

Cited by 24 publications

(21 citation statements)

References 38 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…(iii) Kelvin-Helmholtz instability KH instability is a basic physical process that occurs when there is velocity shear in a single continuous fluid, or when there is a velocity difference across the interface between two fluids [147]. Recent observations have revealed the occurrence of KH instability in the solar atmosphere, such as at the interface between an erupting region and the surrounding corona [148], at the outer edge of CMEs [149], in prominences [150], in coronal streamers [151] and in solar jets [152,153].…”

Section: (Ii) Plasmoidmentioning

confidence: 99%

“…Using IRIS observations, Li et al [152] reported the developing process of KH instability in a blowout jet due to the strong velocity shear of two plasma flows along the jet spire, in which the developing process was about 80 s and the distortion scale was less than 1.6 Mm. Using H α observations taken by the NVST, Yuan et al [153] studied the KH instability at the outer edge of a small solar jet, in which the KH instability was thought to be caused by the shearing motion between cool chromospheric and hot coronal plasma flows. During the mature stage, plasma heating was evidenced around the region of the vortex structures, supporting the scenario that KH instability can effectively transfer plasma kinetic energy into thermal energy and heat the coronal plasma.…”

Section: Observational Featurementioning

confidence: 99%

“…This provided a link between the magnetic activities in the lower atmosphere and coronal heating (figure 11). In addition, solar jets also excite shocks ahead of them and drive KH instability at their boundaries; the dissipation of shocks and reconnection within the vortex structures also releases energy to heat the corona [6,94,153].

Figure 11Heating effect caused by spicular activities [9].…”

Section: Relation To Other Phenomenamentioning

confidence: 99%

See 2 more Smart Citations

Observation and modelling of solar jets

Shen

2021

Proc. R. Soc. A.

Self Cite

View full text Add to dashboard Cite

The solar atmosphere is full of complicated transients manifesting the reconfiguration of the solar magnetic field and plasma. Solar jets represent collimated, beam-like plasma ejections; they are ubiquitous in the solar atmosphere and important for our understanding of solar activities at different scales, the magnetic reconnection process, particle acceleration, coronal heating, solar wind acceleration, as well as other related phenomena. Recent high-spatio-temporal-resolution, wide-temperature coverage and spectroscopic and stereoscopic observations taken by ground-based and space-borne solar telescopes have revealed many valuable new clues to restrict the development of theoretical models. This review aims at providing the reader with the main observational characteristics of solar jets, physical interpretations and models, as well as unsolved outstanding questions in future studies.

show abstract

Section: (Ii) Plasmoidmentioning

confidence: 99%

Section: Observational Featurementioning

confidence: 99%

Figure 11Heating effect caused by spicular activities [9].…”

Section: Relation To Other Phenomenamentioning

confidence: 99%

See 1 more Smart Citation

Observation and modelling of solar jets

Shen

2021

Proc. R. Soc. A.

Self Cite

View full text Add to dashboard Cite

show abstract

“…However, observations of the KHI have been scarce so far, either limited to quiescent prominences (e.g. Berger et al, 2010, see also Section 4.9.3) or to very energetic events, such as CME eruptions (Foullon et al, 2011) or flares (Brannon, Longcope, and Qiu, 2015;Yuan et al, 2019). Observations of the KHI in quiescent prominences with IRIS suggest that only large field-aligned shear flows (with Alfvén Mach number larger than 2) are able to trigger the instability in such conditions (Hillier and Polito, 2018, see also Figure 18 and Section 4.9.3).…”

Section: Fundamental Mhd Instabilitiesmentioning

confidence: 99%

A New View of the Solar Interface Region from the Interface Region Imaging Spectrograph (IRIS)

et al. 2021

View full text Add to dashboard Cite

The Interface Region Imaging Spectrograph (IRIS) has been obtaining near- and far-ultraviolet images and spectra of the solar atmosphere since July 2013. IRIS is the highest resolution observatory to provide seamless coverage of spectra and images from the photosphere into the low corona. The unique combination of near- and far-ultraviolet spectra and images at sub-arcsecond resolution and high cadence allows the tracing of mass and energy through the critical interface between the surface and the corona or solar wind. IRIS has enabled research into the fundamental physical processes thought to play a role in the low solar atmosphere such as ion–neutral interactions, magnetic reconnection, the generation, propagation, and dissipation of waves, the acceleration of non-thermal particles, and various small-scale instabilities. IRIS has provided insights into a wide range of phenomena including the discovery of non-thermal particles in coronal nano-flares, the formation and impact of spicules and other jets, resonant absorption and dissipation of Alfvénic waves, energy release and jet-like dynamics associated with braiding of magnetic-field lines, the role of turbulence and the tearing-mode instability in reconnection, the contribution of waves, turbulence, and non-thermal particles in the energy deposition during flares and smaller-scale events such as UV bursts, and the role of flux ropes and various other mechanisms in triggering and driving CMEs. IRIS observations have also been used to elucidate the physical mechanisms driving the solar irradiance that impacts Earth’s upper atmosphere, and the connections between solar and stellar physics. Advances in numerical modeling, inversion codes, and machine-learning techniques have played a key role. With the advent of exciting new instrumentation both on the ground, e.g. the Daniel K. Inouye Solar Telescope (DKIST) and the Atacama Large Millimeter/submillimeter Array (ALMA), and space-based, e.g. the Parker Solar Probe and the Solar Orbiter, we aim to review new insights based on IRIS observations or related modeling, and highlight some of the outstanding challenges.

show abstract

“…The slow solar wind that emerges from the equatorial region of the Sun is considered to be affected by the turbulent shear source (see Adhikari et al 2020b). Kelvin-Helmholtz instabilities may develop in the inner and outer corona (DeForest et al 2016;Yuan et al 2019), which may provide a source of turbulence shear source close to the Sun (Ruffolo et al 2020) and may affect the slow and fast solar wind from above the sonic point. We will address this issue in a future paper.…”

Section: Solar Wind Plus Ni Mhd Turbulence Transport Modelmentioning

confidence: 99%

Evolution of anisotropic turbulence in the fast and slow solar wind: Theory and Solar Orbiter measurements

Adhikari

Zank

Zhao

et al. 2021

A&A

View full text Add to dashboard Cite

Aims. Solar Orbiter (SolO) was launched on February 9, 2020, allowing us to study the nature of turbulence in the inner heliopshere. We investigate the evolution of anisotropic turbulence in the fast and slow solar wind in the inner heliosphere using the nearly incompressible magnetohydrodynamic (NI MHD) turbulence model and SolO measurements. Methods. We calculated the two dimensional (2D) and the slab variances of the energy in forward and backward propagating modes, the fluctuating magnetic energy, the fluctuating kinetic energy, the normalized residual energy, and the normalized cross-helicity as a function of the angle between the mean solar wind speed and the mean magnetic field (θ U B ), and as a function of the heliocentric distance using SolO measurements. We compared the observed results and the theoretical results of the NI MHD turbulence model as a function of the heliocentric distance. Results. The results show that the ratio of 2D energy and slab energy of forward and backward propagating modes, magnetic field fluctuations, and kinetic energy fluctuations increases as the angle between the mean solar wind flow and the mean magnetic field increases from θ U B = 0 • to approximately θ U B = 90 • and then decreases as θ U B → 180 • . We find that solar wind turbulence is a superposition of the dominant 2D component and a minority slab component as a function of the heliocentric distance. We find excellent agreement between the theoretical results and observed results as a function of the heliocentric distance.

show abstract

Multilayered Kelvin–Helmholtz Instability in the Solar Corona

Cited by 24 publications

References 38 publications

Observation and modelling of solar jets

Observation and modelling of solar jets

A New View of the Solar Interface Region from the Interface Region Imaging Spectrograph (IRIS)

Evolution of anisotropic turbulence in the fast and slow solar wind: Theory and Solar Orbiter measurements

Contact Info

Product

Resources

About